Author: "Smiljanic, R." / Publisher: edp sciences - Searchworks@Jio Institute Digital Library Search Results

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179 results on '"Smiljanic, R."'

1. The Gaia-ESO Survey: No sign of multiple stellar populations in open clusters from their sodium and oxygen abundances.

Author: Bragaglia, A., D'Orazi, V., Magrini, L., Baratella, M., Bensby, T., Martell, S. L., Randich, S., Tautvaišienė, G., Alfaro, E. J., Morbidelli, L., Smiljanic, R., and Zaggia, S.
Subjects: STELLAR dynamics, STELLAR populations, OPEN clusters of stars, MAGELLANIC clouds, STAR formation, GLOBULAR clusters
Abstract: Context. The light element (anti-)correlations shown by globular clusters (GCs) are the main spectroscopic signature of multiple stellar populations. These internal abundance variations provide us with fundamental constraints on the formation mechanism of stellar clusters. Aims. Using Gaia-ESO, the largest and most homogeneous survey of open clusters (OCs), we intend to check whether these stellar aggregates display the same patterns. Based on previous studies of many GCs, several young and massive clusters in the Magellanic Clouds, as well as a few OCs, we do not expect to find any anti-correlation, given the low mass of Milky Way OCs. Methods. We used the results based on UVES spectra of stars in Gaia-ESO to derive the distribution of Na and O abundances and see whether they show an unexplained dispersion or whether they are anti-correlated. By selecting only high-probability members with high-precision stellar parameters, we ended up with more than 700 stars in 74 OCs. We examined the O-Na distribution in 28 OCs with at least 4 stars available as well as the Na distribution in 24 OCs, with at least 10 stars available. Results. We find that the distribution of Na abundances is compatible with a single-value population, within the errors. The few apparent exceptions can be explained by differences in the evolutionary phase (main sequence and giant post first dredge-up episode) or by difficulties in analysing low gravity giants. We did not find any indication of an Na-O anti-correlation in any of the clusters for which O has been derived. Conclusions. Based on the very small spread we find, OCs maintain the status of single stellar populations. However, a definitive answer requires studying more elements and larger samples covering different evolutionary phases. This will be possible with the next generation of large surveys. [ABSTRACT FROM AUTHOR]
Published: 2024
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2. The Gaia-ESO Survey: Calibrating the lithium–age relation with open clusters and associations: II. Expanded cluster sample and final membership selection.

Author: Gutiérrez Albarrán, M. L., Montes, D., Tabernero, H. M., González Hernández, J. I., Marfil, E., Frasca, A., Lanzafame, A. C., Klutsch, A., Franciosini, E., Randich, S., Smiljanic, R., Korn, A. J., Gilmore, G., Alfaro, E. J., Bensby, T., Biazzo, K., Casey, A., Carraro, G., Damiani, F., and Feltzing, S.
Subjects: OPEN clusters of stars, MAIN sequence (Astronomy), STAR clusters, CLUSTER sampling, STELLAR rotation, STARS, AGE of stars
Abstract: Context. The Li abundance observed in pre-main sequence and main sequence late-type stars is strongly age-dependent, but also shows a complex pattern depending on several parameters, such as rotation, chromospheric activity, and metallicity. The best way to calibrate these effects, and with the aim of studying Li as an age indicator for FGK stars, is to calibrate coeval groups of stars, such as open clusters (OCs) and associations. Aims. We present a considerable target sample of 42 OCs and associations – with an age range from 1 Myr to 5 Gyr – observed within the Gaia-ESO survey (GES), and using the latest data provided by GES iDR6 and the most recent release of Gaia that was then available, EDR3. As part of this study, we update and improve the membership analysis for all 20 OCs presented in our previous article. Methods. We perform detailed membership analyses for all target clusters to identify likely candidates, using all available parameters provided by GES, complemented with detailed bibliographical searches, and based on numerous criteria: from radial velocity distributions, to the astrometry (proper motions and parallaxes) and photometry provided by Gaia, to gravity indicators (log g and the γ index), [Fe/H] metallicity, and Li content in diagrams of (Li equivalent widths) EW(Li) versus Teff. Results. We obtain updated lists of cluster members for the whole target sample, as well as a selection of Li-rich giant contaminants obtained as an additional result of the membership process. Each selection of cluster candidates was thoroughly contrasted with numerous existing membership studies using data from Gaia to ensure the most robust results. Conclusions. These final cluster selections will be used in the third and last paper of this series, which reports the results of a comparative study characterising the observable Li dispersion in each cluster and analysing its dependence on several parameters, allowing us to calibrate a Li–age relation and obtain a series of empirical Li envelopes for key ages in our sample. [ABSTRACT FROM AUTHOR]
Published: 2024
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3. The Gaia-ESO Survey: Homogenisation of stellar parameters and elemental abundances

Author: Hourihane, A., primary, François, P., additional, Worley, C. C., additional, Magrini, L., additional, Gonneau, A., additional, Casey, A. R., additional, Gilmore, G., additional, Randich, S., additional, Sacco, G. G., additional, Recio-Blanco, A., additional, Korn, A. J., additional, Allende Prieto, C., additional, Smiljanic, R., additional, Blomme, R., additional, Bragaglia, A., additional, Walton, N. A., additional, Van Eck, S., additional, Bensby, T., additional, Lanzafame, A., additional, Frasca, A., additional, Franciosini, E., additional, Damiani, F., additional, Lind, K., additional, Bergemann, M., additional, Bonifacio, P., additional, Hill, V., additional, Lobel, A., additional, Montes, D., additional, Feuillet, D. K., additional, Tautvaišienė, G., additional, Guiglion, G., additional, Tabernero, H. M., additional, González Hernández, J. I., additional, Gebran, M., additional, Van der Swaelmen, M., additional, Mikolaitis, Š., additional, Daflon, S., additional, Merle, T., additional, Morel, T., additional, Lewis, J. R., additional, González Solares, E. A., additional, Murphy, D. N. A., additional, Jeffries, R. D., additional, Jackson, R. J., additional, Feltzing, S., additional, Prusti, T., additional, Carraro, G., additional, Biazzo, K., additional, Prisinzano, L., additional, Jofré, P., additional, Zaggia, S., additional, Drazdauskas, A., additional, Stonkuté, E., additional, Marfil, E., additional, Jiménez-Esteban, F., additional, Mahy, L., additional, Gutiérrez Albarrán, M. L., additional, Berlanas, S. R., additional, Santos, W., additional, Morbidelli, L., additional, Spina, L., additional, and Minkevičiūtė, R., additional
Published: 2023
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4. Exploring the chemodynamics of metal-poor stellar populations

Author: da Silva, A.R., primary and Smiljanic, R., additional
Published: 2023
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5. The Gaia-ESO Survey: Chemical evolution of Mg and Al in the Milky Way with machine learning

Author: Ambrosch, M., primary, Guiglion, G., additional, Mikolaitis, Š., additional, Chiappini, C., additional, Tautvaišienė, G., additional, Nepal, S., additional, Gilmore, G., additional, Randich, S., additional, Bensby, T., additional, Bayo, A., additional, Bergemann, M., additional, Morbidelli, L., additional, Pancino, E., additional, Sacco, G. G., additional, Smiljanic, R., additional, Zaggia, S., additional, Jofré, P., additional, and Jiménez-Esteban, F. M., additional
Published: 2023
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6. Chronology of the chemical enrichment of the old Galactic stellar populations

Author: Giribaldi, R.E., primary and Smiljanic, R., additional
Published: 2023
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7. The Gaia-ESO Survey: Preparing the ground for 4MOST and WEAVE galactic surveys

Author: Nepal, S., primary, Guiglion, G., additional, de Jong, R. S., additional, Valentini, M., additional, Chiappini, C., additional, Steinmetz, M., additional, Ambrosch, M., additional, Pancino, E., additional, Jeffries, R. D., additional, Bensby, T., additional, Romano, D., additional, Smiljanic, R., additional, Dantas, M. L. L., additional, Gilmore, G., additional, Randich, S., additional, Bayo, A., additional, Bergemann, M., additional, Franciosini, E., additional, Jiménez-Esteban, F., additional, Jofré, P., additional, Morbidelli, L., additional, Sacco, G. G., additional, Tautvaišienė, G., additional, and Zaggia, S., additional
Published: 2023
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8. The Gaia-ESO survey : Placing constraints on the origin of r-process elements

Author: van der Swaelmen, M., Viscasillas Vazquez, C., Cescutti, G., Magrini, L., Cristallo, S., Vescovi, D., Randich, S., Tautvaisiene, G., Bagdonas, V., Bensby, T., Bergemann, M., Bragaglia, A., Drazdauskas, A., Jimenez-Esteban, F., Guiglion, G., Korn, Andreas, Masseron, T., Minkeviiute, R., Smiljanic, R., Spina, L., Stonkute, E., Zaggia, S., van der Swaelmen, M., Viscasillas Vazquez, C., Cescutti, G., Magrini, L., Cristallo, S., Vescovi, D., Randich, S., Tautvaisiene, G., Bagdonas, V., Bensby, T., Bergemann, M., Bragaglia, A., Drazdauskas, A., Jimenez-Esteban, F., Guiglion, G., Korn, Andreas, Masseron, T., Minkeviiute, R., Smiljanic, R., Spina, L., Stonkute, E., and Zaggia, S.
Abstract: Context: A renewed interest in the origin of r-process elements has been stimulated by the multi-messenger observation of the gravitational event GW170817, with the detection of both gravitational waves and electromagnetic waves corresponding to the merger of two neutron stars. Such a phenomenon has been proposed as one of the main sources of the r-process. However, the origin of the r-process elements at different metallicities is still under debate. Aims: We aim at investigate the origin of the r-process elements in the Galactic thin-disc population. Methods: From the sixth internal data release of the Gaia-ESO, we have collected a large sample of Milky Way (MW) thin- and thick-disc stars for which abundances of Eu, O, and Mg are available. The sample consists of members of 62 open clusters (OCs), located at a Galactocentric radius between similar to 5kpc and similar to 20kpc in the disc, in the metallicity range [- 0.5,0.4], and covering an age interval from 0.1 to 7 Gy, and about 1300 Milky Way disc field stars in the metallicity range [- 1.5,0.5]. We compare the observations with the results of a chemical evolution model, in which we varied the nucleosynthesis sources for the three elements considered. Results: Our main result is that Eu in the thin disc is predominantly produced by sources with short lifetimes, such as magneto-rotationally driven SNe. There is no strong evidence for additional sources at delayed times. Conclusions: Our findings do not imply that there cannot be a contribution from mergers of neutron stars in other environments, as in the halo or in dwarf spheroidal galaxies, but such a contribution is not needed to explain Eu abundances at thin-disc metallicities.
Published: 2023
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9. The Gaia-ESO Survey: Homogenisation of stellar parameters and elemental abundances

Author: Universidad de Alicante. Departamento de Física Aplicada, Hourihane, A., François, P., Worley, C.C., Magrini, L., Gonneau, A., Casey, A.R., Gilmore, Gerard, Randich, Sofia, Sacco, G.G., Recio-Blanco, A., Korn, A., Allende Prieto, C., Smiljanic, R., Blomme, Ronny, Bragaglia, A., Walton, N., Van Eck, S., Bensby, T., Lanzafame, A.C., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, Alex, Montes, David, Feuillet, D.K., Tautvaišienė, G., Guiglion, G., Tabernero, Hugo M., González Hernández, J.I., Gebran, M., Van der Swaelmen, M., Mikolaitis, Š., Daflon, Simone, Merle, T., Morel, Thierry, Lewis, J., González Solares, E.A., Murphy, D.N.A., Jeffries, R., Jackson, R.J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkuté, E., Marfil, E., Jiménez Esteban, Francisco M., Mahy, Laurent, Gutiérrez Albarrán, M.L., Berlanas, Sara R., Santos, W., Morbidelli, L., Spina, L., Minkevičiūtė, R., Universidad de Alicante. Departamento de Física Aplicada, Hourihane, A., François, P., Worley, C.C., Magrini, L., Gonneau, A., Casey, A.R., Gilmore, Gerard, Randich, Sofia, Sacco, G.G., Recio-Blanco, A., Korn, A., Allende Prieto, C., Smiljanic, R., Blomme, Ronny, Bragaglia, A., Walton, N., Van Eck, S., Bensby, T., Lanzafame, A.C., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, Alex, Montes, David, Feuillet, D.K., Tautvaišienė, G., Guiglion, G., Tabernero, Hugo M., González Hernández, J.I., Gebran, M., Van der Swaelmen, M., Mikolaitis, Š., Daflon, Simone, Merle, T., Morel, Thierry, Lewis, J., González Solares, E.A., Murphy, D.N.A., Jeffries, R., Jackson, R.J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkuté, E., Marfil, E., Jiménez Esteban, Francisco M., Mahy, Laurent, Gutiérrez Albarrán, M.L., Berlanas, Sara R., Santos, W., Morbidelli, L., Spina, L., and Minkevičiūtė, R.
Abstract: The Gaia-ESO Survey is a public spectroscopic survey that targeted ≳105 stars covering all major components of the Milky Way from the end of 2011 to 2018, delivering its final public release in May 2022. Unlike other spectroscopic surveys, Gaia-ESO is the only survey that observed stars across all spectral types with dedicated, specialised analyses: from O (Teff ~ 30 000–52 000 K) all the way to K-M (≳3500 K). The physics throughout these stellar regimes varies significantly, which has previously prohibited any detailed comparisons between stars of significantly different types. In the final data release (internal data release 6) of the Gaia-ESO Survey, we provide the final database containing a large number of products, such as radial velocities, stellar parameters and elemental abundances, rotational velocity, and also, for example, activity and accretion indicators in young stars and membership probability in star clusters for more than 114 000 stars. The spectral analysis is coordinated by a number of working groups (WGs) within the survey, each specialised in one or more of the various stellar samples. Common targets are analysed across WGs to allow for comparisons (and calibrations) amongst instrumental setups and spectral types. Here we describe the procedures employed to ensure all survey results are placed on a common scale in order to arrive at a single set of recommended results for use by all survey collaborators. We also present some general quality and consistency checks performed on the entirety of the survey results.
Published: 2023

10. The Gaia-ESO survey: Placing constraints on the origin of r-process elements

Author: Van der Swaelmen, M., primary, Viscasillas Vázquez, C., additional, Cescutti, G., additional, Magrini, L., additional, Cristallo, S., additional, Vescovi, D., additional, Randich, S., additional, Tautvaišienė, G., additional, Bagdonas, V., additional, Bensby, T., additional, Bergemann, M., additional, Bragaglia, A., additional, Drazdauskas, A., additional, Jiménez-Esteban, F., additional, Guiglion, G., additional, Korn, A., additional, Masseron, T., additional, Minkeviiūtė, R., additional, Smiljanic, R., additional, Spina, L., additional, Stonkutė, E., additional, and Zaggia, S., additional
Published: 2023
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11. The Gaia-ESO survey: Mapping the shape and evolution of the radial abundance gradients with open clusters

Author: Magrini, L., primary, Viscasillas Vázquez, C., additional, Spina, L., additional, Randich, S., additional, Romano, D., additional, Franciosini, E., additional, Recio-Blanco, A., additional, Nordlander, T., additional, D’Orazi, V., additional, Baratella, M., additional, Smiljanic, R., additional, Dantas, M. L. L., additional, Pasquini, L., additional, Spitoni, E., additional, Casali, G., additional, Van der Swaelmen, M., additional, Bensby, T., additional, Stonkute, E., additional, Feltzing, S., additional, Sacco, G. G., additional, Bragaglia, A., additional, Pancino, E., additional, Heiter, U., additional, Biazzo, K., additional, Gilmore, G., additional, Bergemann, M., additional, Tautvaišienė, G., additional, Worley, C., additional, Hourihane, A., additional, Gonneau, A., additional, and Morbidelli, L., additional
Published: 2023
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12. The Gaia-ESO Survey: Old super-metal-rich visitors from the inner Galaxy

Author: Dantas, M. L. L., primary, Smiljanic, R., additional, Boesso, R., additional, Rocha-Pinto, H. J., additional, Magrini, L., additional, Guiglion, G., additional, Tautvaišienė, G., additional, Gilmore, G., additional, Randich, S., additional, Bensby, T., additional, Bragaglia, A., additional, Bergemann, M., additional, Carraro, G., additional, Jofré, P., additional, and Zaggia, S., additional
Published: 2023
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13. The Gaia-ESO Survey: Probing the lithium abundances in old metal-rich dwarf stars in the solar vicinity

Author: Dantas, M. L. L., primary, Guiglion, G., additional, Smiljanic, R., additional, Romano, D., additional, Magrini, L., additional, Bensby, T., additional, Chiappini, C., additional, Franciosini, E., additional, Nepal, S., additional, Tautvaišienė, G., additional, Gilmore, G., additional, Randich, S., additional, Lanzafame, A. C., additional, Heiter, U., additional, Morbidelli, L., additional, Prisinzano, L., additional, and Zaggia, S., additional
Published: 2022
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14. The Gaia-ESO Survey: Lithium measurements and new curves of growth,

Author: Franciosini, E., primary, Randich, S., additional, de Laverny, P., additional, Biazzo, K., additional, Feuillet, D. K., additional, Frasca, A., additional, Lind, K., additional, Prisinzano, L., additional, Tautvaišiene, G., additional, Lanzafame, A. C., additional, Smiljanic, R., additional, Gonneau, A., additional, Magrini, L., additional, Pancino, E., additional, Guiglion, G., additional, Sacco, G. G., additional, Sanna, N., additional, Gilmore, G., additional, Bonifacio, P., additional, Jeffries, R. D., additional, Micela, G., additional, Prusti, T., additional, Alfaro, E. J., additional, Bensby, T., additional, Bragaglia, A., additional, François, P., additional, Korn, A. J., additional, Van Eck, S., additional, Bayo, A., additional, Bergemann, M., additional, Carraro, G., additional, Heiter, U., additional, Hourihane, A., additional, Jofré, P., additional, Lewis, J., additional, Martayan, C., additional, Monaco, L., additional, Morbidelli, L., additional, Worley, C. C., additional, and Zaggia, S., additional
Published: 2022
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15. The Gaia-ESO Survey: Chemical tagging in the thin disk

Author: Spina, L., primary, Magrini, L., additional, Sacco, G. G., additional, Casali, G., additional, Vallenari, A., additional, Tautvaišienė, G., additional, Jiménez-Esteban, F., additional, Gilmore, G., additional, Randich, S., additional, Feltzing, S., additional, Jeffries, R. D., additional, Bensby, T., additional, Bragaglia, A., additional, Smiljanic, R., additional, Carraro, G., additional, Morbidelli, L., additional, and Zaggia, S., additional
Published: 2022
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16. The Gaia-ESO Public Spectroscopic Survey: Implementation, data products, open cluster survey, science, and legacy

Author: Randich, S., primary, Gilmore, G., additional, Magrini, L., additional, Sacco, G. G., additional, Jackson, R. J., additional, Jeffries, R. D., additional, Worley, C. C., additional, Hourihane, A., additional, Gonneau, A., additional, Viscasillas Vazquez, C., additional, Franciosini, E., additional, Lewis, J. R., additional, Alfaro, E. J., additional, Allende Prieto, C., additional, Bensby, T., additional, Blomme, R., additional, Bragaglia, A., additional, Flaccomio, E., additional, François, P., additional, Irwin, M. J., additional, Koposov, S. E., additional, Korn, A. J., additional, Lanzafame, A. C., additional, Pancino, E., additional, Recio-Blanco, A., additional, Smiljanic, R., additional, Van Eck, S., additional, Zwitter, T., additional, Asplund, M., additional, Bonifacio, P., additional, Feltzing, S., additional, Binney, J., additional, Drew, J., additional, Ferguson, A. M. N., additional, Micela, G., additional, Negueruela, I., additional, Prusti, T., additional, Rix, H.-W., additional, Vallenari, A., additional, Bayo, A., additional, Bergemann, M., additional, Biazzo, K., additional, Carraro, G., additional, Casey, A. R., additional, Damiani, F., additional, Frasca, A., additional, Heiter, U., additional, Hill, V., additional, Jofré, P., additional, de Laverny, P., additional, Lind, K., additional, Marconi, G., additional, Martayan, C., additional, Masseron, T., additional, Monaco, L., additional, Morbidelli, L., additional, Prisinzano, L., additional, Sbordone, L., additional, Sousa, S. G., additional, Zaggia, S., additional, Adibekyan, V., additional, Bonito, R., additional, Caffau, E., additional, Daflon, S., additional, Feuillet, D. K., additional, Gebran, M., additional, Gonzalez Hernandez, J. I., additional, Guiglion, G., additional, Herrero, A., additional, Lobel, A., additional, Maiz Apellaniz, J., additional, Merle, T., additional, Mikolaitis, Š., additional, Montes, D., additional, Morel, T., additional, Soubiran, C., additional, Spina, L., additional, Tabernero, H. M., additional, Tautvaišiene, G., additional, Traven, G., additional, Valentini, M., additional, Van der Swaelmen, M., additional, Villanova, S., additional, Wright, N. J., additional, Abbas, U., additional, Aguirre Børsen-Koch, V., additional, Alves, J., additional, Balaguer-Nunez, L., additional, Barklem, P. S., additional, Barrado, D., additional, Berlanas, S. R., additional, Binks, A. S., additional, Bressan, A., additional, Capuzzo-Dolcetta, R., additional, Casagrande, L., additional, Casamiquela, L., additional, Collins, R. S., additional, D'Orazi, V., additional, Dantas, M. L. L., additional, Debattista, V. P., additional, Delgado-Mena, E., additional, Di Marcantonio, P., additional, Drazdauskas, A., additional, Evans, N. W., additional, Famaey, B., additional, Franchini, M., additional, Frémat, Y., additional, Friel, E. D., additional, Fu, X., additional, Geisler, D., additional, Gerhard, O., additional, Gonzalez Solares, E. A., additional, Grebel, E. K., additional, Gutierrez Albarran, M. L., additional, Hatzidimitriou, D., additional, Held, E. V., additional, Jiménez-Esteban, F., additional, Jönsson, H., additional, Jordi, C., additional, Khachaturyants, T., additional, Kordopatis, G., additional, Kos, J., additional, Lagarde, N., additional, Mahy, L., additional, Mapelli, M., additional, Marfil, E., additional, Martell, S. L., additional, Messina, S., additional, Miglio, A., additional, Minchev, I., additional, Moitinho, A., additional, Montalban, J., additional, Monteiro, M. J. P. F. G., additional, Morossi, C., additional, Mowlavi, N., additional, Mucciarelli, A., additional, Murphy, D. N. A., additional, Nardetto, N., additional, Ortolani, S., additional, Paletou, F., additional, Palouš, J., additional, Paunzen, E., additional, Pickering, J. C., additional, Quirrenbach, A., additional, Re Fiorentin, P., additional, Read, J. I., additional, Romano, D., additional, Ryde, N., additional, Sanna, N., additional, Santos, W., additional, Seabroke, G. M., additional, Spagna, A., additional, Steinmetz, M., additional, Stonkuté, E., additional, Sutorius, E., additional, Thévenin, F., additional, Tosi, M., additional, Tsantaki, M., additional, Vink, J. S., additional, Wright, N., additional, Wyse, R. F. G., additional, Zoccali, M., additional, Zorec, J., additional, Zucker, D. B., additional, and Walton, N. A., additional
Published: 2022
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17. The Gaia-ESO Public Spectroscopic Survey: Motivation, implementation, GIRAFFE data processing, analysis, and final data products

Author: Gilmore, G., primary, Randich, S., additional, Worley, C. C., additional, Hourihane, A., additional, Gonneau, A., additional, Sacco, G. G., additional, Lewis, J. R., additional, Magrini, L., additional, François, P., additional, Jeffries, R. D., additional, Koposov, S. E., additional, Bragaglia, A., additional, Alfaro, E. J., additional, Allende Prieto, C., additional, Blomme, R., additional, Korn, A. J., additional, Lanzafame, A. C., additional, Pancino, E., additional, Recio-Blanco, A., additional, Smiljanic, R., additional, Van Eck, S., additional, Zwitter, T., additional, Bensby, T., additional, Flaccomio, E., additional, Irwin, M. J., additional, Franciosini, E., additional, Morbidelli, L., additional, Damiani, F., additional, Bonito, R., additional, Friel, E. D., additional, Vink, J. S., additional, Prisinzano, L., additional, Abbas, U., additional, Hatzidimitriou, D., additional, Held, E. V., additional, Jordi, C., additional, Paunzen, E., additional, Spagna, A., additional, Jackson, R. J., additional, Maíz Apellániz, J., additional, Asplund, M., additional, Bonifacio, P., additional, Feltzing, S., additional, Binney, J., additional, Drew, J., additional, Ferguson, A. M. N., additional, Micela, G., additional, Negueruela, I., additional, Prusti, T., additional, Rix, H.-W., additional, Vallenari, A., additional, Bergemann, M., additional, Casey, A. R., additional, de Laverny, P., additional, Frasca, A., additional, Hill, V., additional, Lind, K., additional, Sbordone, L., additional, Sousa, S. G., additional, Adibekyan, V., additional, Caffau, E., additional, Daflon, S., additional, Feuillet, D. K., additional, Gebran, M., additional, Gonzalez Hernandez, J. I., additional, Guiglion, G., additional, Herrero, A., additional, Lobel, A., additional, Merle, T., additional, Mikolaitis, Š., additional, Montes, D., additional, Morel, T., additional, Ruchti, G., additional, Soubiran, C., additional, Tabernero, H. M., additional, Tautvaišienė, G., additional, Traven, G., additional, Valentini, M., additional, Van der Swaelmen, M., additional, Villanova, S., additional, Viscasillas Vázquez, C., additional, Bayo, A., additional, Biazzo, K., additional, Carraro, G., additional, Edvardsson, B., additional, Heiter, U., additional, Jofré, P., additional, Marconi, G., additional, Martayan, C., additional, Masseron, T., additional, Monaco, L., additional, Walton, N. A., additional, Zaggia, S., additional, Aguirre Børsen-Koch, V., additional, Alves, J., additional, Balaguer-Nunez, L., additional, Barklem, P. S., additional, Barrado, D., additional, Bellazzini, M., additional, Berlanas, S. R., additional, Binks, A. S., additional, Bressan, A., additional, Capuzzo-Dolcetta, R., additional, Casagrande, L., additional, Casamiquela, L., additional, Collins, R. S., additional, D'Orazi, V., additional, Dantas, M. L. L., additional, Debattista, V. P., additional, Delgado-Mena, E., additional, Di Marcantonio, P., additional, Drazdauskas, A., additional, Evans, N. W., additional, Famaey, B., additional, Franchini, M., additional, Frémat, Y., additional, Fu, X., additional, Geisler, D., additional, Gerhard, O., additional, González Solares, E. A., additional, Grebel, E. K., additional, Gutiérrez Albarrán, M. L., additional, Jiménez-Esteban, F., additional, Jönsson, H., additional, Khachaturyants, T., additional, Kordopatis, G., additional, Kos, J., additional, Lagarde, N., additional, Ludwig, H.-G., additional, Mahy, L., additional, Mapelli, M., additional, Marfil, E., additional, Martell, S. L., additional, Messina, S., additional, Miglio, A., additional, Minchev, I., additional, Moitinho, A., additional, Montalban, J., additional, Monteiro, M. J. P. F. G., additional, Morossi, C., additional, Mowlavi, N., additional, Mucciarelli, A., additional, Murphy, D. N. A., additional, Nardetto, N., additional, Ortolani, S., additional, Paletou, F., additional, Palouš, J., additional, Pickering, J. C., additional, Quirrenbach, A., additional, Re Fiorentin, P., additional, Read, J. I., additional, Romano, D., additional, Ryde, N., additional, Sanna, N., additional, Santos, W., additional, Seabroke, G. M., additional, Spina, L., additional, Steinmetz, M., additional, Stonkuté, E., additional, Sutorius, E., additional, Thévenin, F., additional, Tosi, M., additional, Tsantaki, M., additional, Wright, N., additional, Wyse, R. F. G., additional, Zoccali, M., additional, Zorec, J., additional, and Zucker, D. B., additional
Published: 2022
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18. The Gaia-ESO Survey: Target selection of open cluster stars & x22c6;

Author: Bragaglia, A., Alfaro, E. J., Flaccomio, E., Blomme, R., Donati, P., Costado, M., Damiani, F., Franciosini, E., Prisinzano, L., Randich, S., Friel, E. D., Hatztidimitriou, D., Vallenari, A., Spagna, A., Balaguer-Nunez, L., Bonito, R., Gaudin, T. Cantat, Casamiquela, L., Jeffries, R. D., Jordi, C., Magrini, L., Drew, J. E., Jackson, R. J., Abbas, U., Caramazza, M., Hayes, C., Jimenez-Esteban, F. M., Fiorentin, P. Re, Wright, N., Bayo, A., Bensb, T., Bergemann, M., Gilmore, G., Gonneau, A., Heiter, Ulrike, Hourihane, A., Pancino, E., Sacco, G., Smiljanic, R., Zaggia, S., and Vink, J. S.
Subjects: stars, abundances, open clusters and associations, kinematics and dynamics, spectroscopic, surveys, Astronomi, astrofysik och kosmologi, general, Astronomy, Astrophysics and Cosmology, techniques, radial velocities, QB600, QB, QB799
Abstract: Context. The Gaia-ESO Survey (GES) is a public, high-resolution spectroscopic survey, conducted with the multi-object spectrograph Fibre Large Array Multi Element Spectrograph (FLAMES) on the Very Large Telescope (European Southern Observatory, ESO, Cerro Paranal, Chile) from December 2011 to January 2018. Gaia-ESO has targeted all the main stellar components of the Milky Way, including thin and thick disc, bulge, and halo. In particular, a large sample of open clusters has been observed, from very young ones, just out of the embedded phase, to very old ones.\ud \ud Aims. The different kinds of clusters and stars targeted in them are useful to reach the main science goals of the open cluster part of GES, which are the study of the open cluster structure and dynamics, the use of open clusters to constrain and improve stellar evolution models, and the definition of Galactic disc properties (e.g., metallicity distribution).\ud \ud Methods. The Gaia-ESO Survey is organised in 19 working groups (WGs), each one being responsible for a task. We describe here the work of three of them, one in charge of the selection of the targets within each cluster or association (WG4), one responsible for defining the most probable candidate member stars (WG1), and another one in charge of the preparation of the observations (WG6). As the entire GES has been conducted before the second Gaia data release, we could not make use of the Gaia astrometry to define cluster member candidates. We made use of public and private photometry to select the stars to be observed with FLAMES, once brought on a common astrometric system (the one defined by 2MASS). Candidate target selection was based on ground-based proper motions, radial velocities, and X-ray properties when appropriate, for example, and it was mostly used to define the position of the clusters’ evolutionary sequences in the colour-magnitude diagrams. Targets for GIRAFFE were then selected near the sequences in an unbiased way. We used known information on membership, when available, only for the few stars to be observed with UVES.\ud \ud Results. We collected spectra for 62 confirmed clusters in the main observing campaign (and a few more clusters were taken from the ESO archive). Among them are very young clusters, where the main targets are pre-main sequence stars, clusters with very hot and massive stars currently on the main sequence, intermediate-age and old clusters where evolved stars are the main targets. Our strategy of making the selection of targets as inclusive and unbiased as possible and of observing a significant and representative fraction of all possible targets permitted us to collect the largest, most accurate, and most homogeneous spectroscopic data set on open star clusters ever achieved.
Published: 2022

19. The Gaia-ESO Survey: The analysis of the hot-star spectra

Author: Universidad de Alicante. Departamento de Física Aplicada, Blomme, Ronny, Daflon, Simone, Gebran, M., Herrero, Artemio, Lobel, Alex, Mahy, Laurent, Martins, Fabrice, Morel, Thierry, Berlanas, Sara R., Blazère, A., Frémat, Y., Gosset, E., Maíz Apellániz, Jesús, Santos, W., Semaan, T., Simón Díaz, Sergio, Volpi, D., Holgado, Gonzalo, Jiménez Esteban, Francisco M., Nieva, M.F., Przybilla, Norbert, Gilmore, Gerard, Randich, Sofia, Negueruela, Ignacio, Prusti, T., Vallenari, A., Alfaro, Emilio J., Bensby, T., Bragaglia, A., Flaccomio, E., Francois, P., Korn, A., Lanzafame, A.C., Pancino, E., Smiljanic, R., Bergemann, M., Carraro, G., Franciosini, E., Gonneau, A., Heiter, U., Hourihane, A., Jofre, P., Magrini, L., Morbidelli, L., Sacco, G.G., Worley, C.C., Zaggia, S., Universidad de Alicante. Departamento de Física Aplicada, Blomme, Ronny, Daflon, Simone, Gebran, M., Herrero, Artemio, Lobel, Alex, Mahy, Laurent, Martins, Fabrice, Morel, Thierry, Berlanas, Sara R., Blazère, A., Frémat, Y., Gosset, E., Maíz Apellániz, Jesús, Santos, W., Semaan, T., Simón Díaz, Sergio, Volpi, D., Holgado, Gonzalo, Jiménez Esteban, Francisco M., Nieva, M.F., Przybilla, Norbert, Gilmore, Gerard, Randich, Sofia, Negueruela, Ignacio, Prusti, T., Vallenari, A., Alfaro, Emilio J., Bensby, T., Bragaglia, A., Flaccomio, E., Francois, P., Korn, A., Lanzafame, A.C., Pancino, E., Smiljanic, R., Bergemann, M., Carraro, G., Franciosini, E., Gonneau, A., Heiter, U., Hourihane, A., Jofre, P., Magrini, L., Morbidelli, L., Sacco, G.G., Worley, C.C., and Zaggia, S.
Abstract: Context. The Gaia-ESO Survey (GES) is a large public spectroscopic survey that has collected, over a period of six years, spectra of ~105 stars. This survey provides not only the reduced spectra, but also the stellar parameters and abundances resulting from the analysis of the spectra. Aims. The GES dataflow is organised in 19 working groups. Working group 13 (WG13) is responsible for the spectral analysis of the hottest stars (O, B, and A type, with a formal cutoff of Teff > 7000 K) that were observed as part of GES. We present the procedures and techniques that have been applied to the reduced spectra in order to determine the stellar parameters and abundances of these stars. Methods. The procedure used was similar to that of other working groups in GES. A number of groups (called Nodes) each independently analyse the spectra via state-of-the-art techniques and codes. Specific for the analysis in WG13 was the large temperature range covered (Teff ≈ 7000–50 000 K), requiring the use of different analysis codes. Most Nodes could therefore only handle part of the data. Quality checks were applied to the results of these Nodes by comparing them to benchmark stars, and by comparing them to one another. For each star the Node values were then homogenised into a single result: the recommended parameters and abundances. Results. Eight Nodes each analysed part of the data. In total 17 693 spectra of 6462 stars were analysed, most of them in 37 open star clusters. The homogenisation led to stellar parameters for 5584 stars. Abundances were determined for a more limited number of stars. The elements studied are He, C, N, O, Ne, Mg, Al, Si, and Sc. Abundances for at least one of these elements were determined for 292 stars. Conclusions. The hot-star data analysed here, as well as the GES data in general, will be of considerable use in future studies of stellar evolution and open clusters.
Published: 2022

20. The Gaia-ESO Survey : The analysis of the hot-star spectra

Author: Blomme, R., Daflon, S., Gebran, M., Herrero, A., Lobel, A., Mahy, L., Martins, F., Morel, T., Berlanas, S. R., Blazere, A., Fremat, Y., Gosset, E., Apellaniz, J. Maiz, Santos, W., Semaan, T., Simon-Diaz, S., Volpi, D., Holgado, G., Jimenez-Esteban, F., Nieva, M. F., Przybilla, N., Gilmore, G., Randich, S., Negueruela, I, Prusti, T., Vallenari, A., Alfaro, E. J., Bensby, T., Bragaglia, A., Flaccomio, E., Francois, P., Korn, Andreas, Lanzafame, A., Pancino, E., Smiljanic, R., Bergemann, M., Carraro, G., Franciosini, E., Gonneau, A., Heiter, Ulrike, Hourihane, A., Jofre, P., Magrini, L., Morbidelli, L., Sacco, G. G., Worley, C. C., Zaggia, S., Blomme, R., Daflon, S., Gebran, M., Herrero, A., Lobel, A., Mahy, L., Martins, F., Morel, T., Berlanas, S. R., Blazere, A., Fremat, Y., Gosset, E., Apellaniz, J. Maiz, Santos, W., Semaan, T., Simon-Diaz, S., Volpi, D., Holgado, G., Jimenez-Esteban, F., Nieva, M. F., Przybilla, N., Gilmore, G., Randich, S., Negueruela, I, Prusti, T., Vallenari, A., Alfaro, E. J., Bensby, T., Bragaglia, A., Flaccomio, E., Francois, P., Korn, Andreas, Lanzafame, A., Pancino, E., Smiljanic, R., Bergemann, M., Carraro, G., Franciosini, E., Gonneau, A., Heiter, Ulrike, Hourihane, A., Jofre, P., Magrini, L., Morbidelli, L., Sacco, G. G., Worley, C. C., and Zaggia, S.
Abstract: Context. The Gaia-ESO Survey (GES) is a large public spectroscopic survey that has collected, over a period of six years, spectra of similar to 10(5) stars. This survey provides not only the reduced spectra, but also the stellar parameters and abundances resulting from the analysis of the spectra. Aims. The GES dataflow is organised in 19 working groups. Working group 13 (WG13) is responsible for the spectral analysis of the hottest stars (O, B, and A type, with a formal cutoff of T-eff > 7000 K) that were observed as part of GES. We present the procedures and techniques that have been applied to the reduced spectra in order to determine the stellar parameters and abundances of these stars. Methods. The procedure used was similar to that of other working groups in GES. A number of groups (called Nodes) each independently analyse the spectra via state-of-the-art techniques and codes. Specific for the analysis in WG13 was the large temperature range covered (T-eff approximate to 7000-50 000 K), requiring the use of different analysis codes. Most Nodes could therefore only handle part of the data. Quality checks were applied to the results of these Nodes by comparing them to benchmark stars, and by comparing them to one another. For each star the Node values were then homogenised into a single result: the recommended parameters and abundances. Results. Eight Nodes each analysed part of the data. In total 17 693 spectra of 6462 stars were analysed, most of them in 37 open star clusters. The homogenisation led to stellar parameters for 5584 stars. Abundances were determined for a more limited number of stars. The elements studied are He, C, N, O, Ne, Mg, Al, Si, and Sc. Abundances for at least one of these elements were determined for 292 stars. Conclusions. The hot-star data analysed here, as well as the GES data in general, will be of considerable use in future studies of stellar evolution and open clusters.
Published: 2022
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21. The Gaia-ESO survey : Age-chemical-clock relations spatially resolved in the Galactic disc

Author: Viscasillas Vazquez, C., Magrini, L., Casali, G., Tautvaisiene, G., Spina, L., van der Swaelmen, M., Randich, S., Bensby, T., Bragaglia, A., Friel, E., Feltzing, S., Sacco, G. G., Turchi, A., Jimenez-Esteban, F., D'Orazi, V., Delgado-Mena, E., Mikolaitis, S., Drazdauskas, A., Minkeviciute, R., Stonkute, E., Bagdonas, V., Montes, D., Guiglion, G., Baratella, M., Tabernero, H. M., Gilmore, G., Alfaro, E., Francois, P., Korn, Andreas, Smiljanic, R., Bergemann, M., Franciosini, E., Gonneau, A., Hourihane, A., Worley, C. C., Zaggia, S., Viscasillas Vazquez, C., Magrini, L., Casali, G., Tautvaisiene, G., Spina, L., van der Swaelmen, M., Randich, S., Bensby, T., Bragaglia, A., Friel, E., Feltzing, S., Sacco, G. G., Turchi, A., Jimenez-Esteban, F., D'Orazi, V., Delgado-Mena, E., Mikolaitis, S., Drazdauskas, A., Minkeviciute, R., Stonkute, E., Bagdonas, V., Montes, D., Guiglion, G., Baratella, M., Tabernero, H. M., Gilmore, G., Alfaro, E., Francois, P., Korn, Andreas, Smiljanic, R., Bergemann, M., Franciosini, E., Gonneau, A., Hourihane, A., Worley, C. C., and Zaggia, S.
Abstract: Context. The last decade has seen a revolution in our knowledge of the Galaxy thanks to the Gaia and asteroseismic space missions and the ground-based spectroscopic surveys. Aims. To complete this picture, it is necessary to map the ages of its stellar populations. During recent years, the dependence on time of abundance ratios involving slow (s) neutron-capture and ff elements (called chemical-clocks) has been used to provide estimates of stellar ages, usually in a limited volume close to the Sun. We aim to analyse the relations of chemical clocks in the Galactic disc extending the range to R-GC similar to 6-20 kpc. Methods. Using the sixth internal data release of the Gaia-ESO survey, we calibrated several relations between stellar ages and abundance ratios [s/alpha] using a sample of open clusters, the largest one so far used with this aim (62 clusters). Thanks to their wide galactocentric coverage, we investigated the radial variations of the shape of these relations, confirming their non-universality. Results. The multi-variate relations allowed us to infer stellar ages for field stars. We estimated our accuracy (ranging from 0.0 to -0.9 Gyr) and precision (from 0.4 to 2.3 Gyr) in recovering the global ages of open clusters, and the ages of their individual members. We applied the relations with the highest correlation coe fficients to the field star population, finding an older population at lower metallicity and higher [alpha/Fe] in the thin disc, and a younger one at higher [Fe/H] and low [alpha/Fe], as expected. Conclusion. We confirm that there is no single age-chemical clock relationship valid for the whole disc, but that there is a dependence on the galactocentric position, which is related to the radial variation of the star formation history combined with the non-monotonic dependence on metallicity of the yields of the s-process elements from low- and intermediate-mass stars. Finally, the abundance ratios [Ba/alpha] are more sensitive to age than those
Published: 2022
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22. Gaia-ESO Survey : Detailed elemental abundances in red giants of the peculiar globular cluster NGC 1851

Author: Tautvaisiene, G., Drazdauskas, A., Bragaglia, A., Martell, S. L., Pancino, E., Lardo, C., Mikolaitis, S., Minkeviciute, R., Stonkute, E., Ambrosch, M., Bagdonas, V., Chorniy, Y., Sanna, N., Franciosini, E., Smiljanic, R., Randich, S., Gilmore, G., Bensby, T., Bergemann, M., Gonneau, A., Guiglion, G., Carraro, G., Heiter, Ulrike, Korn, Andreas, Magrini, L., Morbidelli, L., Zaggia, S., Tautvaisiene, G., Drazdauskas, A., Bragaglia, A., Martell, S. L., Pancino, E., Lardo, C., Mikolaitis, S., Minkeviciute, R., Stonkute, E., Ambrosch, M., Bagdonas, V., Chorniy, Y., Sanna, N., Franciosini, E., Smiljanic, R., Randich, S., Gilmore, G., Bensby, T., Bergemann, M., Gonneau, A., Guiglion, G., Carraro, G., Heiter, Ulrike, Korn, Andreas, Magrini, L., Morbidelli, L., and Zaggia, S.
Abstract: Context. NGC 1851 is one of several globular clusters for which multiple stellar populations of the subgiant branch have been clearly identified and a difference in metallicity detected. A crucial piece of information on the formation history of this cluster can be provided by the sum of A(C+N+O) abundances. However, these values have lacked a general consensus thus far. The separation of the subgiant branch can be based on age and/or A(C+N+O) abundance differences. Aims. Our main aim was to determine carbon, nitrogen, and oxygen abundances for evolved giants in the globular cluster NGC 1851 in order to check whether or not the double populations of stars are coeval. Methods. High-resolution spectra, observed with the FLAMES-UVES spectrograph on the ESO VLT telescope, were analysed using a differential model atmosphere method. Abundances of carbon were derived using spectral synthesis of the C-2 band heads at 5135 and 5635.5 angstrom. The wavelength interval 6470-6490 angstrom, with CN features, was analysed to determine nitrogen abundances. Oxygen abundances were determined from the [OI] line at 6300 angstrom. Abundances of other chemical elements were determined from equivalent widths or spectral syntheses of unblended spectral lines. Results. We provide abundances of up to 29 chemical elements for a sample of 45 giants in NGC 1851. The investigated stars can be separated into two populations with a difference of 0.07 dex in the mean metallicity, 0.3 dex in the mean C/N, and 0.35 dex in the mean s-process dominated element-to-iron abundance ratios [s/Fe]. No significant difference was determined in the mean values of A(C+N+O) as well as in abundance to iron ratios of carbon, alpha- and iron-peak-elements, and of europium. Conclusions. As the averaged A(C+N+O) values between the two populations do not differ, additional evidence is given that NGC 1851 is composed of two clusters, the metal-rich cluster being by about 0.6 Gyr older than the metal-poor one. A global
Published: 2022
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23. The Gaia-ESO Survey: Lithium measurements and new curves of growth

Author: Ministerio de Ciencia e Innovación (España), European Commission, European Research Council, Franciosini, E., Randich, S., de Laverny, P., Biazzo, K., Feuillet, D. K., Frasca, A., Lind, K., Prisinzano, L., Tautvaišiene, G., Lanzafame, A. C., Smiljanic, R., Gonneau, A., Magrini, L., Pancino, E., Guiglion, Guillaume, Sacco, G. G., Sanna, N., Gilmore, Gerry, Bonifacio, P., Jeffries, R. D., Micela, Giusi, Prusti, T., Alfaro, Emilio J., Bensby, T., Bragaglia, A., François, P., Korn, A. J., Van Eck, S., Bayo, A., Bergemann, Maria, Carraro, G., Heiter, Ulrike, Hourihane, A., Jofré, P., Lewis, J., Martayan, C., Monaco, L., Morbidelli, L., Worley, C. C., Zaggia, S., Ministerio de Ciencia e Innovación (España), European Commission, European Research Council, Franciosini, E., Randich, S., de Laverny, P., Biazzo, K., Feuillet, D. K., Frasca, A., Lind, K., Prisinzano, L., Tautvaišiene, G., Lanzafame, A. C., Smiljanic, R., Gonneau, A., Magrini, L., Pancino, E., Guiglion, Guillaume, Sacco, G. G., Sanna, N., Gilmore, Gerry, Bonifacio, P., Jeffries, R. D., Micela, Giusi, Prusti, T., Alfaro, Emilio J., Bensby, T., Bragaglia, A., François, P., Korn, A. J., Van Eck, S., Bayo, A., Bergemann, Maria, Carraro, G., Heiter, Ulrike, Hourihane, A., Jofré, P., Lewis, J., Martayan, C., Monaco, L., Morbidelli, L., Worley, C. C., and Zaggia, S.
Abstract: Context. The Gaia-ESO Survey (GES) is a large public spectroscopic survey that was carried out using the multi-object FLAMES spectrograph at the Very Large Telescope. The survey provides accurate radial velocities, stellar parameters, and elemental abundances for ~115 000 stars in all Milky Way components. Aims. In this paper, we describe the method adopted in the final data release to derive lithium equivalent widths (EWs) and abundances. Methods. Lithium EWs were measured using two different approaches for FGK and M-type stars, to account for the intrinsic differences in the spectra. For FGK stars, we fitted the lithium line using Gaussian components, while direct integration over a predefined interval was adopted for M-type stars. Care was taken to ensure continuity between the two regimes. Abundances were derived using a new set of homogeneous curves of growth that were derived specifically for GES, and which were measured on a synthetic spectral grid consistently with the way the EWs were measured. The derived abundances were validated by comparison with those measured by other analysis groups using different methods. Results. Lithium EWs were measured for ~40 000 stars, and abundances could be derived for ~38 000 of them. The vast majority of the measures (80%) have been obtained for stars in open cluster fields. The remaining objects are stars in globular clusters, or field stars in the Milky Way disc, bulge, and halo. Conclusions. The GES dataset of homogeneous lithium abundances described here will be valuable for our understanding of several processes, from stellar evolution and internal mixing in stars at different evolutionary stages to Galactic evolution. © E. Franciosini et al. 2022.
Published: 2022

24. The Gaia-ESO Public Spectroscopic Survey: Implementation, data products, open cluster survey, science, and legacy

Author: Universidad de Alicante. Departamento de Física Aplicada, Randich, Sofia, Gilmore, Gerard, Magrini, L., Sacco, G.G., Jackson, R.J., Jeffries, R., Worley, C.C., Hourihane, A., Gonneau, A., Viscasillas Vázquez, C., Franciosini, E., Sbordone, L., Sousa, S.G., Zaggia, S., Adibekyan, V.Zh., Bonito, R., Caffau, E., Daflon, Simone, Feuillet, D.K., Drazdauskas, A., Gebran, M., Lagarde, N., González Hernández, J.I., Guiglion, G., Herrero, Artemio, Lobel, Alex, Maíz Apellániz, Jesús, Merle, T., Mikolaitis, Š., Montes, David, Morel, Thierry, Evans, N.W., Mahy, Laurent, Soubiran, C., Spina, L., Tabernero, Hugo M., Tautvaišienė, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Wright, N.J., Abbas, U., Mapelli, M., Famaey, B., Aguirre Børsen-Koch, V., Alves, J., Balaguer-Nunez, L., Barklem, P.S., Barrado, D., Berlanas, Sara R., Binks, A.S., Bressan, A., Capuzzo-Dolcetta, R., Marfil, E., Casagrande, L., Franchini, M., Casamiquela, L., Collins, R.S., D'Orazi, V., Dantas, M.L.L., Debattista, V.P., Frémat, Y., Friel, E., Fu, X., Martell, S.L., Geisler, Douglas, Lewis, J., Gerhard, Ortwin, González Solares, E.A., Grebel, E.K., Gutiérrez Albarran, M.L., Hatzidimitriou, D., Held, E.V., Jiménez Esteban, Francisco M., Jönsson, H., Messina, S., Jordi, C., Khachaturyants, T., Alfaro, Emilio J., Kordopatis, G., Kos, J., Miglio, A., Minchev, I., Allende Prieto, C., Moitinho, A., Negueruela, Ignacio, Montalban, J., Monteiro, M.J.P.F.G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D.N.A., Nardetto, N., Ortolani, S., Paletou, F., Bensby, T., Prusti, T., Palouš, J., Paunzen, E., Pickering, J.C., Quirrenbach, A., Re Fiorentin, P., Read, J.I., Romano, D., Ryde, N., Sanna, N., Santos, W., Rix, H.-W., Blomme, Ronny, Seabroke, G.M., Spagna, A., Steinmetz, M., Stonkuté, E., Sutorius, E., Thévenin, F., Tosi, M., Tsantaki, M., Vink, Jorick S., Vallenari, A., Wright, N., Bragaglia, A., Wyse, R.F.G., Zoccali, M., Zorec, J., Zucker, D.B., Walton, N., Flaccomio, E., François, P., Irwin, M., Bayo, A., Koposov, S., Korn, A., Lanzafame, A.C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Asplund, M., Bonifacio, P., Bergemann, M., Feltzing, S., Binney, J., Drew, J., Ferguson, A., Micela, G., Biazzo, K., Carraro, G., Casey, A.R., Damiani, F., Delgado-Mena, E., Frasca, A., Heiter, U., Hill, V., Jofre, P., Laverny, P. de, Lind, K., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Di Marcantonio, P., Morbidelli, L., Prisinzano, L., Universidad de Alicante. Departamento de Física Aplicada, Randich, Sofia, Gilmore, Gerard, Magrini, L., Sacco, G.G., Jackson, R.J., Jeffries, R., Worley, C.C., Hourihane, A., Gonneau, A., Viscasillas Vázquez, C., Franciosini, E., Sbordone, L., Sousa, S.G., Zaggia, S., Adibekyan, V.Zh., Bonito, R., Caffau, E., Daflon, Simone, Feuillet, D.K., Drazdauskas, A., Gebran, M., Lagarde, N., González Hernández, J.I., Guiglion, G., Herrero, Artemio, Lobel, Alex, Maíz Apellániz, Jesús, Merle, T., Mikolaitis, Š., Montes, David, Morel, Thierry, Evans, N.W., Mahy, Laurent, Soubiran, C., Spina, L., Tabernero, Hugo M., Tautvaišienė, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Wright, N.J., Abbas, U., Mapelli, M., Famaey, B., Aguirre Børsen-Koch, V., Alves, J., Balaguer-Nunez, L., Barklem, P.S., Barrado, D., Berlanas, Sara R., Binks, A.S., Bressan, A., Capuzzo-Dolcetta, R., Marfil, E., Casagrande, L., Franchini, M., Casamiquela, L., Collins, R.S., D'Orazi, V., Dantas, M.L.L., Debattista, V.P., Frémat, Y., Friel, E., Fu, X., Martell, S.L., Geisler, Douglas, Lewis, J., Gerhard, Ortwin, González Solares, E.A., Grebel, E.K., Gutiérrez Albarran, M.L., Hatzidimitriou, D., Held, E.V., Jiménez Esteban, Francisco M., Jönsson, H., Messina, S., Jordi, C., Khachaturyants, T., Alfaro, Emilio J., Kordopatis, G., Kos, J., Miglio, A., Minchev, I., Allende Prieto, C., Moitinho, A., Negueruela, Ignacio, Montalban, J., Monteiro, M.J.P.F.G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D.N.A., Nardetto, N., Ortolani, S., Paletou, F., Bensby, T., Prusti, T., Palouš, J., Paunzen, E., Pickering, J.C., Quirrenbach, A., Re Fiorentin, P., Read, J.I., Romano, D., Ryde, N., Sanna, N., Santos, W., Rix, H.-W., Blomme, Ronny, Seabroke, G.M., Spagna, A., Steinmetz, M., Stonkuté, E., Sutorius, E., Thévenin, F., Tosi, M., Tsantaki, M., Vink, Jorick S., Vallenari, A., Wright, N., Bragaglia, A., Wyse, R.F.G., Zoccali, M., Zorec, J., Zucker, D.B., Walton, N., Flaccomio, E., François, P., Irwin, M., Bayo, A., Koposov, S., Korn, A., Lanzafame, A.C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Asplund, M., Bonifacio, P., Bergemann, M., Feltzing, S., Binney, J., Drew, J., Ferguson, A., Micela, G., Biazzo, K., Carraro, G., Casey, A.R., Damiani, F., Delgado-Mena, E., Frasca, A., Heiter, U., Hill, V., Jofre, P., Laverny, P. de, Lind, K., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Di Marcantonio, P., Morbidelli, L., and Prisinzano, L.
Abstract: Context. In the last 15 years different ground-based spectroscopic surveys have been started (and completed) with the general aim of delivering stellar parameters and elemental abundances for large samples of Galactic stars, complementing Gaia astrometry. Among those surveys, the Gaia-ESO Public Spectroscopic Survey, the only one performed on a 8m class telescope, was designed to target 100 000 stars using FLAMES on the ESO VLT (both Giraffe and UVES spectrographs), covering all the Milky Way populations, with a special focus on open star clusters. Aims. This article provides an overview of the survey implementation (observations, data quality, analysis and its success, data products, and releases), of the open cluster survey, of the science results and potential, and of the survey legacy. A companion article reviews the overall survey motivation, strategy, Giraffe pipeline data reduction, organisation, and workflow. Methods. We made use of the information recorded and archived in the observing blocks; during the observing runs; in a number of relevant documents; in the spectra and master catalogue of spectra; in the parameters delivered by the analysis nodes and the working groups; in the final catalogue; and in the science papers. Based on these sources, we critically analyse and discuss the output and products of the Survey, including science highlights. We also determined the average metallicities of the open clusters observed as science targets and of a sample of clusters whose spectra were retrieved from the ESO archive. Results. The Gaia-ESO Survey has determined homogeneous good-quality radial velocities and stellar parameters for a large fraction of its more than 110 000 unique target stars. Elemental abundances were derived for up to 31 elements for targets observed with UVES. Lithium abundances are delivered for about 1/3 of the sample. The analysis and homogenisation strategies have proven to be successful; several science topics have been addressed by t
Published: 2022

25. The Gaia-ESO Public Spectroscopic Survey: Motivation, implementation, GIRAFFE data processing, analysis, and final data products

Author: Universidad de Alicante. Departamento de Física Aplicada, Gilmore, Gerard, Randich, Sofia, Worley, C.C., Hourihane, A., Gonneau, A., Sacco, G.G., Lewis, J., Magrini, L., François, P., Jeffries, R., Koposov, S., Binks, A.S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R.S., D'Orazi, V., Dantas, M.L.L., Debattista, V.P., Delgado-Mena, E., Bragaglia, A., Di Marcantonio, P., Drazdauskas, A., Evans, N.W., Famaey, B., Franchini, M., Frémat, Y., Fu, X., Geisler, Douglas, Gerhard, Ortwin, González Solares, E.A., Alfaro, Emilio J., Grebel, E.K., Gutiérrez Albarrán, M.L., Jiménez Esteban, Francisco M., Jönsson, H., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H.-G., Mahy, Laurent, Allende Prieto, C., Mapelli, M., Marfil, E., Martell, S.L., Messina, S., Miglio, A., Minchev, I., Moitinho, A., Montalban, J., Monteiro, M.J.P.F.G., Morossi, C., Blomme, Ronny, Mowlavi, N., Mucciarelli, A., Murphy, D.N.A., Nardetto, N., Ortolani, S., Paletou, F., Palouš, J., Pickering, J.C., Quirrenbach, A., Re Fiorentin, P., Korn, A., Read, J.I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G.M., Spina, L., Steinmetz, M., Stonkuté, E., Sutorius, E., Lanzafame, A.C., Thévenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R.F.G., Zoccali, M., Zorec, J., Zucker, D.B., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E., Vink, Jorick S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E.V., Jordi, C., Paunzen, E., Spagna, A., Jackson, R.J., Maíz Apellániz, Jesús, Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A., Micela, G., Negueruela, Ignacio, Prusti, T., Rix, H.-W., Vallenari, A., Bergemann, M., Casey, A.R., Laverny, P. de, Frasca, A., Hill, V., Lind, K., Sbordone, L., Sousa, S.G., Adibekyan, V.Zh., Caffau, E., Daflon, Simone, Feuillet, D.K., Gebran, M., González Hernández, J.I., Guiglion, G., Herrero, Artemio, Lobel, Alex, Merle, T., Mikolaitis, Š., Montes, David, Morel, Thierry, Ruchti, G., Soubiran, C., Tabernero, Hugo M., Tautvaišienė, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Viscasillas Vázquez, C., Bayo, A., Biazzo, K., Carraro, G., Edvardsson, B., Heiter, U., Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N., Zaggia, S., Aguirre Børsen-Koch, V., Alves, J., Balaguer-Nunez, L., Barklem, P.S., Barrado, D., Bellazzini, M., Berlanas, Sara R., Universidad de Alicante. Departamento de Física Aplicada, Gilmore, Gerard, Randich, Sofia, Worley, C.C., Hourihane, A., Gonneau, A., Sacco, G.G., Lewis, J., Magrini, L., François, P., Jeffries, R., Koposov, S., Binks, A.S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R.S., D'Orazi, V., Dantas, M.L.L., Debattista, V.P., Delgado-Mena, E., Bragaglia, A., Di Marcantonio, P., Drazdauskas, A., Evans, N.W., Famaey, B., Franchini, M., Frémat, Y., Fu, X., Geisler, Douglas, Gerhard, Ortwin, González Solares, E.A., Alfaro, Emilio J., Grebel, E.K., Gutiérrez Albarrán, M.L., Jiménez Esteban, Francisco M., Jönsson, H., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H.-G., Mahy, Laurent, Allende Prieto, C., Mapelli, M., Marfil, E., Martell, S.L., Messina, S., Miglio, A., Minchev, I., Moitinho, A., Montalban, J., Monteiro, M.J.P.F.G., Morossi, C., Blomme, Ronny, Mowlavi, N., Mucciarelli, A., Murphy, D.N.A., Nardetto, N., Ortolani, S., Paletou, F., Palouš, J., Pickering, J.C., Quirrenbach, A., Re Fiorentin, P., Korn, A., Read, J.I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G.M., Spina, L., Steinmetz, M., Stonkuté, E., Sutorius, E., Lanzafame, A.C., Thévenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R.F.G., Zoccali, M., Zorec, J., Zucker, D.B., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E., Vink, Jorick S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E.V., Jordi, C., Paunzen, E., Spagna, A., Jackson, R.J., Maíz Apellániz, Jesús, Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A., Micela, G., Negueruela, Ignacio, Prusti, T., Rix, H.-W., Vallenari, A., Bergemann, M., Casey, A.R., Laverny, P. de, Frasca, A., Hill, V., Lind, K., Sbordone, L., Sousa, S.G., Adibekyan, V.Zh., Caffau, E., Daflon, Simone, Feuillet, D.K., Gebran, M., González Hernández, J.I., Guiglion, G., Herrero, Artemio, Lobel, Alex, Merle, T., Mikolaitis, Š., Montes, David, Morel, Thierry, Ruchti, G., Soubiran, C., Tabernero, Hugo M., Tautvaišienė, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Viscasillas Vázquez, C., Bayo, A., Biazzo, K., Carraro, G., Edvardsson, B., Heiter, U., Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N., Zaggia, S., Aguirre Børsen-Koch, V., Alves, J., Balaguer-Nunez, L., Barklem, P.S., Barrado, D., Bellazzini, M., and Berlanas, Sara R.
Abstract: Context. The Gaia-ESO Public Spectroscopic Survey is an ambitious project designed to obtain astrophysical parameters and elemental abundances for 100 000 stars, including large representative samples of the stellar populations in the Galaxy, and a well-defined sample of 60 (plus 20 archive) open clusters. We provide internally consistent results calibrated on benchmark stars and star clusters, extending across a very wide range of abundances and ages. This provides a legacy data set of intrinsic value, and equally a large wide-ranging dataset that is of value for the homogenisation of other and future stellar surveys and Gaia's astrophysical parameters. Aims. This article provides an overview of the survey methodology, the scientific aims, and the implementation, including a description of the data processing for the GIRAFFE spectra. A companion paper introduces the survey results. Methods. Gaia-ESO aspires to quantify both random and systematic contributions to measurement uncertainties. Thus, all available spectroscopic analysis techniques are utilised, each spectrum being analysed by up to several different analysis pipelines, with considerable effort being made to homogenise and calibrate the resulting parameters. We describe here the sequence of activities up to delivery of processed data products to the ESO Science Archive Facility for open use. Results. The Gaia-ESO Survey obtained 202 000 spectra of 115 000 stars using 340 allocated VLT nights between December 2011 and January 2018 from GIRAFFE and UVES. Conclusions. The full consistently reduced final data set of spectra was released through the ESO Science Archive Facility in late 2020, with the full astrophysical parameters sets following in 2022. A companion article reviews the survey implementation, scientific highlights, the open cluster survey, and data products.
Published: 2022

26. The Gaia-ESO Survey: Target selection of open cluster stars

Author: Ministerio de Ciencia e Innovación (España), Junta de Andalucía, European Commission, Bragaglia, A., Alfaro, Emilio J., Flaccomio, E., Blomme, R., Donati, P., Costado, M. T., Damiani, F., Franciosini, E., Prisinzano, L., Randich, S., Friel, E. D., Hatztidimitriou, D., Vallenari, A., Spagna, A., Balaguer-Nuñez, Lola, Bonito, R., Cantat-Gaudin, Tristan, Casamiquela, Laia, Jeffries, R.D., Jordi, Carme, Magrini, Laura, Drew, J. E., Jackson, R. J., Abbas, U., Caramazza, M., Hayes, C., Jiménez-Esteban, Francisco M., Re Fiorentin, P., Wright, N., Bayo, A., Bensby, T., Bergemann, Maria, Gilmore, Gerry, Gonneau, A., Heiter, Ulrike, Hourihane, A., Pancino, E., Sacco, G., Smiljanic, R., Zaggia, S., Vink, J. S., Ministerio de Ciencia e Innovación (España), Junta de Andalucía, European Commission, Bragaglia, A., Alfaro, Emilio J., Flaccomio, E., Blomme, R., Donati, P., Costado, M. T., Damiani, F., Franciosini, E., Prisinzano, L., Randich, S., Friel, E. D., Hatztidimitriou, D., Vallenari, A., Spagna, A., Balaguer-Nuñez, Lola, Bonito, R., Cantat-Gaudin, Tristan, Casamiquela, Laia, Jeffries, R.D., Jordi, Carme, Magrini, Laura, Drew, J. E., Jackson, R. J., Abbas, U., Caramazza, M., Hayes, C., Jiménez-Esteban, Francisco M., Re Fiorentin, P., Wright, N., Bayo, A., Bensby, T., Bergemann, Maria, Gilmore, Gerry, Gonneau, A., Heiter, Ulrike, Hourihane, A., Pancino, E., Sacco, G., Smiljanic, R., Zaggia, S., and Vink, J. S.
Abstract: Context. The Gaia-ESO Survey (GES) is a public, high-resolution spectroscopic survey, conducted with the multi-object spectrograph Fibre Large Array Multi Element Spectrograph (FLAMES) on the Very Large Telescope (European Southern Observatory, ESO, Cerro Paranal, Chile) from December 2011 to January 2018. Gaia-ESO has targeted all the main stellar components of the Milky Way, including thin and thick disc, bulge, and halo. In particular, a large sample of open clusters has been observed, from very young ones, just out of the embedded phase, to very old ones. Aims. The different kinds of clusters and stars targeted in them are useful to reach the main science goals of the open cluster part of GES, which are the study of the open cluster structure and dynamics, the use of open clusters to constrain and improve stellar evolution models, and the definition of Galactic disc properties (e.g., metallicity distribution). Methods. The Gaia-ESO Survey is organised in 19 working groups (WGs), each one being responsible for a task. We describe here the work of three of them, one in charge of the selection of the targets within each cluster or association (WG4), one responsible for defining the most probable candidate member stars (WG1), and another one in charge of the preparation of the observations (WG6). As the entire GES has been conducted before the second Gaia data release, we could not make use of the Gaia astrometry to define cluster member candidates. We made use of public and private photometry to select the stars to be observed with FLAMES, once brought on a common astrometric system (the one defined by 2MASS). Candidate target selection was based on ground-based proper motions, radial velocities, and X-ray properties when appropriate, for example, and it was mostly used to define the position of the clusters’ evolutionary sequences in the colour-magnitude diagrams. Targets for GIRAFFE were then selected near the sequences in an unbiased way. We used known informati
Published: 2022

27. Gaia-ESO Survey: Chemical evolution of Mg and Al in the Milky Way with machine learning.

Author: Ambrosch, M., Guiglion, G., Mikolaitis, Š., Chiappini, C., Tautvaišiené, G., Nepal, S., Gilmore, G., Randich, S., Bensby, T., Bayo, A., Bergemann, M., Morbidelli, L., Pancino, E., Sacco, G. G., Smiljanic, R., Zaggia, S., Jofré, P., and Jiménez-Esteban, F. M.
Subjects: MACHINE learning, MILKY Way, CONVOLUTIONAL neural networks, STELLAR populations, DATA release, STELLAR spectra
Abstract: Context. To take full advantage of upcoming large-scale spectroscopic surveys, it will be necessary to parameterize millions of stellar spectra in an effcient way. Machine learning methods, especially convolutional neural networks (CNNs), will be among the main tools geared at achieving this task. Aims. We aim to prepare the groundwork for machine learning techniques for the next generation of spectroscopic surveys, such as 4MOST and WEAVE. Our goal is to show that CNNs can predict accurate stellar labels from relevant spectral features in a physically meaningful way. The predicted labels can be used to investigate properties of the Milky Way galaxy. Methods. We built a neural network and trained it on GIRAFFE spectra with their associated stellar labels from the sixth internal Gaia-ESO data release. Our network architecture contains several convolutional layers that allow the network to identify absorption features in the input spectra. The internal uncertainty was estimated from multiple network models. We used the t-distributed stochastic neighbor embedding tool to remove bad spectra from our training sample. Results. Our neural network is able to predict the atmospheric parameters Te and log(g) as well as the chemical abundances [Mg/Fe], [Al/Fe], and [Fe/H] for 36 904 stellar spectra. The training precision is 37K for Te, 0.06 dex for log(g), 0.05 dex for [Mg/Fe], 0.08 dex for [Al/Fe], and 0.04 dex for [Fe/H]. Network gradients reveal that the network is inferring the labels in a physically meaningful way from spectral features. We validated our methodology using benchmark stars and recovered the properties of different stellar populations in the Milky Way galaxy. Conclusions. Such a study provides very good insights into the application of machine learning for the analysis of large-scale spectroscopic surveys, such as WEAVE and 4MOST MilkyWay disk and bulge low- and high-resolution (4MIDABLE-LR and -HR). The community will have to put substantial efforts into building proactive training sets for machine learning methods to minimize any possible systematics. [ABSTRACT FROM AUTHOR]
Published: 2023
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28. The Gaia-ESO Survey: The analysis of the hot-star spectra

Author: Blomme, R., primary, Daflon, S., additional, Gebran, M., additional, Herrero, A., additional, Lobel, A., additional, Mahy, L., additional, Martins, F., additional, Morel, T., additional, Berlanas, S. R., additional, Blazère, A., additional, Frémat, Y., additional, Gosset, E., additional, Maíz Apellániz, J., additional, Santos, W., additional, Semaan, T., additional, Simón-Díaz, S., additional, Volpi, D., additional, Holgado, G., additional, Jiménez-Esteban, F., additional, Nieva, M. F., additional, Przybilla, N., additional, Gilmore, G., additional, Randich, S., additional, Negueruela, I., additional, Prusti, T., additional, Vallenari, A., additional, Alfaro, E. J., additional, Bensby, T., additional, Bragaglia, A., additional, Flaccomio, E., additional, Francois, P., additional, Korn, A. J., additional, Lanzafame, A., additional, Pancino, E., additional, Smiljanic, R., additional, Bergemann, M., additional, Carraro, G., additional, Franciosini, E., additional, Gonneau, A., additional, Heiter, U., additional, Hourihane, A., additional, Jofré, P., additional, Magrini, L., additional, Morbidelli, L., additional, Sacco, G. G., additional, Worley, C. C., additional, and Zaggia, S., additional
Published: 2022
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29. The Gaia-ESO survey: Age-chemical-clock relations spatially resolved in the Galactic disc

Author: Viscasillas Vázquez, C., primary, Magrini, L., additional, Casali, G., additional, Tautvaišienė, G., additional, Spina, L., additional, Van der Swaelmen, M., additional, Randich, S., additional, Bensby, T., additional, Bragaglia, A., additional, Friel, E., additional, Feltzing, S., additional, Sacco, G.G., additional, Turchi, A., additional, Jiménez-Esteban, F., additional, D’Orazi, V., additional, Delgado-Mena, E., additional, Mikolaitis, Š., additional, Drazdauskas, A., additional, Minkevičiūtė, R., additional, Stonkutė, E., additional, Bagdonas, V., additional, Montes, D., additional, Guiglion, G., additional, Baratella, M., additional, Tabernero, H. M., additional, Gilmore, G., additional, Alfaro, E., additional, Francois, P., additional, Korn, A., additional, Smiljanic, R., additional, Bergemann, M., additional, Franciosini, E., additional, Gonneau, A., additional, Hourihane, A., additional, Worley, C. C., additional, and Zaggia, S., additional
Published: 2022
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30. The Gaia-ESO Survey: Target selection of open cluster stars

Author: Bragaglia, A., primary, Alfaro, E. J., additional, Flaccomio, E., additional, Blomme, R., additional, Donati, P., additional, Costado, M., additional, Damiani, F., additional, Franciosini, E., additional, Prisinzano, L., additional, Randich, S., additional, Friel, E. D., additional, Hatztidimitriou, D., additional, Vallenari, A., additional, Spagna, A., additional, Balaguer-Nunez, L., additional, Bonito, R., additional, Cantat Gaudin, T., additional, Casamiquela, L., additional, Jeffries, R. D., additional, Jordi, C., additional, Magrini, L., additional, Drew, J. E., additional, Jackson, R. J., additional, Abbas, U., additional, Caramazza, M., additional, Hayes, C., additional, Jiménez-Esteban, F. M., additional, Re Fiorentin, P., additional, Wright, N., additional, Bayo, A., additional, Bensby, T., additional, Bergemann, M., additional, Gilmore, G., additional, Gonneau, A., additional, Heiter, U., additional, Hourihane, A., additional, Pancino, E., additional, Sacco, G., additional, Smiljanic, R., additional, Zaggia, S., additional, and Vink, J. S., additional
Published: 2022
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31. Gaia-ESO Survey: Role of magnetic activity and starspots on pre-main-sequence lithium evolution

Author: Franciosini, E., primary, Tognelli, E., additional, Degl’Innocenti, S., additional, Prada Moroni, P. G., additional, Randich, S., additional, Sacco, G. G., additional, Magrini, L., additional, Pancino, E., additional, Lanzafame, A. C., additional, Smiljanic, R., additional, Prisinzano, L., additional, Sanna, N., additional, Roccatagliata, V., additional, Bonito, R., additional, de Laverny, P., additional, Gutiérrez Albarrán, M. L., additional, Montes, D., additional, Jiménez-Esteban, F., additional, Gilmore, G., additional, Bergemann, M., additional, Carraro, G., additional, Damiani, F., additional, Gonneau, A., additional, Hourihane, A., additional, Morbidelli, L., additional, Worley, C. C., additional, and Zaggia, S., additional
Published: 2022
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32. Gaia-ESO Survey: Detailed elemental abundances in red giants of the peculiar globular cluster NGC 1851

Author: Tautvaišienė, G., primary, Drazdauskas, A., additional, Bragaglia, A., additional, Martell, S. L., additional, Pancino, E., additional, Lardo, C., additional, Mikolaitis, Š., additional, Minkevičiūtė, R., additional, Stonkutė, E., additional, Ambrosch, M., additional, Bagdonas, V., additional, Chorniy, Y., additional, Sanna, N., additional, Franciosini, E., additional, Smiljanic, R., additional, Randich, S., additional, Gilmore, G., additional, Bensby, T., additional, Bergemann, M., additional, Gonneau, A., additional, Guiglion, G., additional, Carraro, G., additional, Heiter, U., additional, Korn, A., additional, Magrini, L., additional, Morbidelli, L., additional, and Zaggia, S., additional
Published: 2022
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33. Gaia-ESO survey: Lithium abundances in open cluster Red Clump stars

Author: Magrini, L., primary, Smiljanic, R., additional, Franciosini, E., additional, Pasquini, L., additional, Randich, S., additional, Casali, G., additional, Viscasillas Vázquez, C., additional, Bragaglia, A., additional, Spina, L., additional, Biazzo, K., additional, Tautvaišienė, G., additional, Masseron, T., additional, Van der Swaelmen, M., additional, Pancino, E., additional, Jiménez-Esteban, F., additional, Guiglion, G., additional, Martell, S., additional, Bensby, T., additional, D’Orazi, V., additional, Baratella, M., additional, Korn, A., additional, Jofre, P., additional, Gilmore, G., additional, Worley, C., additional, Hourihane, A., additional, Gonneau, A., additional, Sacco, G. G., additional, and Morbidelli, L., additional
Published: 2021
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34. The Gaia-ESO Survey: a new approach to chemically characterising young open clusters

Author: Baratella, M., primary, D’Orazi, V., additional, Sheminova, V., additional, Spina, L., additional, Carraro, G., additional, Gratton, R., additional, Magrini, L., additional, Randich, S., additional, Lugaro, M., additional, Pignatari, M., additional, Romano, D., additional, Biazzo, K., additional, Bragaglia, A., additional, Casali, G., additional, Desidera, S., additional, Frasca, A., additional, de Silva, G., additional, Melo, C., additional, Van der Swaelmen, M., additional, Tautvaišienė, G., additional, Jiménez-Esteban, F. M., additional, Gilmore, G., additional, Bensby, T., additional, Smiljanic, R., additional, Bayo, A., additional, Franciosini, E., additional, Gonneau, A., additional, Hourihane, A., additional, Jofré, P., additional, Monaco, L., additional, Morbidelli, L., additional, Sacco, G., additional, Sbordone, L., additional, Worley, C., additional, and Zaggia, S., additional
Published: 2021
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35. The Gaia-ESO Survey: Galactic evolution of lithium from iDR6

Author: Romano, D., primary, Magrini, L., additional, Randich, S., additional, Casali, G., additional, Bonifacio, P., additional, Jeffries, R. D., additional, Matteucci, F., additional, Franciosini, E., additional, Spina, L., additional, Guiglion, G., additional, Chiappini, C., additional, Mucciarelli, A., additional, Ventura, P., additional, Grisoni, V., additional, Bellazzini, M., additional, Bensby, T., additional, Bragaglia, A., additional, de Laverny, P., additional, Korn, A. J., additional, Martell, S. L., additional, Tautvaišienė, G., additional, Carraro, G., additional, Gonneau, A., additional, Jofré, P., additional, Pancino, E., additional, Smiljanic, R., additional, Vallenari, A., additional, Fu, X., additional, Gutiérrez Albarrán, M. L., additional, Jiménez-Esteban, F. M., additional, Montes, D., additional, Damiani, F., additional, Bergemann, M., additional, and Worley, C., additional
Published: 2021
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36. TITANS metal-poor reference stars

Author: Giribaldi, R. E., primary, da Silva, A. R., additional, Smiljanic, R., additional, and Cornejo Espinoza, D., additional
Published: 2021
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37. The Gaia-ESO Survey : Calibrating the lithium-age relation with open clusters and associations I. Cluster age range and initial membership selections

Author: Gutierrez Albarran, M. L., Montes, D., Gomez Garrido, M., Tabernero, H. M., Gonzalez Hernandez, J. , I, Marfil, E., Frasca, A., Lanzafame, A. C., Klutsch, A., Franciosini, E., Randich, S., Smiljanic, R., Korn, Andreas, Gilmore, G., Alfaro, E. J., Baratella, M., Bayo, A., Bensby, T., Bonito, R., Carraro, G., Delgado Mena, E., Feltzing, S., Gonneau, A., Heiter, Ulrike, Hourihane, A., Jimenez Esteban, F., Jofre, P., Masseron, T., Monaco, L., Morbidelli, L., Prisinzano, L., Roccatagliata, V, Sousa, S., Van der Swaelmen, M., Worley, C. C., Zaggia, S., Gutierrez Albarran, M. L., Montes, D., Gomez Garrido, M., Tabernero, H. M., Gonzalez Hernandez, J. , I, Marfil, E., Frasca, A., Lanzafame, A. C., Klutsch, A., Franciosini, E., Randich, S., Smiljanic, R., Korn, Andreas, Gilmore, G., Alfaro, E. J., Baratella, M., Bayo, A., Bensby, T., Bonito, R., Carraro, G., Delgado Mena, E., Feltzing, S., Gonneau, A., Heiter, Ulrike, Hourihane, A., Jimenez Esteban, F., Jofre, P., Masseron, T., Monaco, L., Morbidelli, L., Prisinzano, L., Roccatagliata, V, Sousa, S., Van der Swaelmen, M., Worley, C. C., and Zaggia, S.
Abstract: Context: Previous studies of open clusters have shown that lithium depletion is not only strongly age dependent but also shows a complex pattern with other parameters that is not yet understood. For pre- and main-sequence late-type stars, these parameters include metallicity, mixing mechanisms, convection structure, rotation, and magnetic activity. Aims: We perform a thorough membership analysis for a large number of stars observed within the Gaia-ESO survey (GES) in the field of 20 open clusters, ranging in age from young clusters and associations, to intermediate-age and old open clusters. Methods: Based on the parameters derived from the GES spectroscopic observations, we obtained lists of candidate members for each of the clusters in the sample by deriving radial velocity distributions and studying the position of the kinematic selections in the EW(Li)-versus-T-eff plane to obtain lithium members. We used gravity indicators to discard field contaminants and studied [Fe/H] metallicity to further confirm the membership of the candidates. We also made use of studies using recent data from the Gaia DR1 and DR2 releases to assess our member selections. Results: We identified likely member candidates for the sample of 20 clusters observed in GES (iDR4) with UVES and GIRAFFE, and conducted a comparative study that allowed us to characterize the properties of these members as well as identify field contaminant stars, both lithium-rich giants and non-giant outliers. Conclusions: This work is the first step towards the calibration of the lithium-age relation and its dependence on other GES parameters. During this project we aim to use this relation to infer the ages of GES field stars, and identify their potential membership to young associations and stellar kinematic groups of different ages.
Published: 2020
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38. The Gaia -ESO survey: 3D NLTE abundances in the open cluster NGC 2420 suggest atomic diffusion and turbulent mixing are at the origin of chemical abundance variations

Author: Southern California Earthquake Center, Science and Technology Facilities Council (UK), Leverhulme Trust, European Research Council, European Science Foundation, German Research Foundation, Centre National D'Etudes Spatiales (France), Ministero dell'Istruzione, dell'Università e della Ricerca, Istituto Nazionale di Astrofisica, Instituto Nacional de Ciência e Tecnologia (Brasil), European Commission, Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, Knut and Alice Wallenberg Foundation, Swedish Research Council, Semenova, E., Bergemann, Maria, Deal, M., Serenelli, Aldo, Hansen, Camilla Juul, Gallagher, Austin J., Bayo, A., Bensby, T., Bragaglia, A., Carraro, Giovanni, Morbidelli, L., Pancino, E., Smiljanic, R., Southern California Earthquake Center, Science and Technology Facilities Council (UK), Leverhulme Trust, European Research Council, European Science Foundation, German Research Foundation, Centre National D'Etudes Spatiales (France), Ministero dell'Istruzione, dell'Università e della Ricerca, Istituto Nazionale di Astrofisica, Instituto Nacional de Ciência e Tecnologia (Brasil), European Commission, Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, Knut and Alice Wallenberg Foundation, Swedish Research Council, Semenova, E., Bergemann, Maria, Deal, M., Serenelli, Aldo, Hansen, Camilla Juul, Gallagher, Austin J., Bayo, A., Bensby, T., Bragaglia, A., Carraro, Giovanni, Morbidelli, L., Pancino, E., and Smiljanic, R.
Abstract: Atomic diusion and mixing processes in stellar interiors influence the structure and the surface composition of stars. Some of these processes cannot yet be modelled from the first principles, and they require calibrations. This limits their applicability in stellar models used for studies of stellar populations and Galactic evolution. Aims. Our main goal is to put constraints on the stellar structure and evolution models using new refined measurements of the chemical composition in stars of a Galactic open cluster. Methods.We used medium-resolution, 19 200 R 21 500, optical spectra of stars in the open cluster NGC2420 obtained within the Gaia-ESO survey. The sample covers all evolutionary stages from the main sequence to the red giant branch. Stellar parameters were derived using a combined Bayesian analysis of spectra, 2MASS photometry, and astrometric data from Gaia DR2. The abundances of Mg, Ca, Fe, and Li were determined from non-local thermodynamic equilibrium (NLTE) synthetic spectra, which were computed using one-dimensional (1D) and averaged three-dimensional (3D) model atmospheres. We compare our results with a grid of Code d'Evolution Stellaire Adaptatif et Modulaire (CESTAM) stellar evolution models, which include atomic diusion, turbulent, and rotational mixing. Results. We find prominent evolutionary trends in the abundances of Fe, Ca, Mg, and Li with the mass of the stars in the cluster. Furthermore, Fe, Mg, and Ca show a depletion at the cluster turn-o, but the abundances gradually increase and flatten near the base of the red giant branch. The abundance trend for Li displays a signature of rotational mixing on the main sequence and abrupt depletion on the sub-giant branch, which is caused by advection of Li-poor material to the surface. The analysis of abundances combined with the CESTAM model predictions allows us to place limits on the parameter space of the models and to constrain the zone in the stellar interior, where turbulent mixing takes pla
Published: 2020

39. The Gaia -ESO survey: The non-universality of the age-chemical-clocks-metallicity relations in the Galactic disc

Author: Science and Technology Facilities Council (UK), European Research Council, Leverhulme Trust, Istituto Nazionale di Astrofisica, Ministerio de Economía y Competitividad (España), European Commission, Knut and Alice Wallenberg Foundation, Australian Research Council, Swedish National Space Agency, Swedish Research Council, Casali, G., Spina, Lorenzo, Magrini, L., Karakas, A. I., Kobayashi, C., Casey, A. R., Feltzing, S., Van der Swaelmen, M., Tsantaki, M., Jofré, P., Bragaglia, A., Feuillet, Diane, Bensby, T., Biazzo, K., Gonneau, A., Tautvaišienė, G., Baratella, M., Roccatagliata, V., Pancino, E., Sousa, S., Adibekyan, V., Martell, S., Bayo, A., Jackson, R. J., Jeffries, R.D., Gilmore, Gerry, Randich, S., Alfaro, Emilio J., Koposov, S.E., Korn, A.J., Recio-Blanco, A., Smiljanic, R., Franciosini, E., Hourihane, A., Monaco, L., Morbidelli, L., Sacco, G., Worley, C., Zaggia, S., Science and Technology Facilities Council (UK), European Research Council, Leverhulme Trust, Istituto Nazionale di Astrofisica, Ministerio de Economía y Competitividad (España), European Commission, Knut and Alice Wallenberg Foundation, Australian Research Council, Swedish National Space Agency, Swedish Research Council, Casali, G., Spina, Lorenzo, Magrini, L., Karakas, A. I., Kobayashi, C., Casey, A. R., Feltzing, S., Van der Swaelmen, M., Tsantaki, M., Jofré, P., Bragaglia, A., Feuillet, Diane, Bensby, T., Biazzo, K., Gonneau, A., Tautvaišienė, G., Baratella, M., Roccatagliata, V., Pancino, E., Sousa, S., Adibekyan, V., Martell, S., Bayo, A., Jackson, R. J., Jeffries, R.D., Gilmore, Gerry, Randich, S., Alfaro, Emilio J., Koposov, S.E., Korn, A.J., Recio-Blanco, A., Smiljanic, R., Franciosini, E., Hourihane, A., Monaco, L., Morbidelli, L., Sacco, G., Worley, C., and Zaggia, S.
Abstract: Context. In the era of large spectroscopic surveys, massive databases of high-quality spectra coupled with the products of the Gaia satellite provide tools to outline a new picture of our Galaxy. In this framework, an important piece of information is provided by our ability to infer stellar ages, and consequently to sketch a Galactic timeline. Aims. We aim to provide empirical relations between stellar ages and abundance ratios for a sample of stars with very similar stellar parameters to those of the Sun, namely the so-called solar-like stars. We investigate the dependence on metallicity, and we apply our relations to independent samples, that is, the Gaia-ESO samples of open clusters and of field stars. Methods. We analyse high-resolution and high-signal-to-noise-ratio HARPS spectra of a sample of solar-like stars to obtain precise determinations of their atmospheric parameters and abundances for 25 elements and/or ions belonging to the main nucleosynthesis channels through differential spectral analysis, and of their ages through isochrone fitting. Results. We investigate the relations between stellar ages and several abundance ratios. For the abundance ratios with a steeper dependence on age, we perform multivariate linear regressions, in which we include the dependence on metallicity, [Fe/H]. We apply our best relations to a sample of open clusters located from the inner to the outer regions of the Galactic disc. Using our relations, we are able to recover the literature ages only for clusters located at RGC&Rlarr2; > &Rlarr2; 7 kpc. The values that we obtain for the ages of the inner-disc clusters are much greater than the literature ones. In these clusters, the content of neutron capture elements, such as Y and Zr, is indeed lower than expected from chemical evolution models, and consequently their [Y/Mg] and [Y/Al] are lower than in clusters of the same age located in the solar neighbourhood. With our chemical evolution model and a set of empirical yields
Published: 2020

40. Inhomogeneity in the early Galactic chemical enrichment exposed by beryllium abundances in extremely metal-poor stars

Author: Smiljanic, R., primary, Zych, M. G., additional, and Pasquini, L., additional
Published: 2021
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41. Atomic data for the Gaia-ESO Survey

Author: Heiter, U., primary, Lind, K., additional, Bergemann, M., additional, Asplund, M., additional, Mikolaitis, Š., additional, Barklem, P. S., additional, Masseron, T., additional, de Laverny, P., additional, Magrini, L., additional, Edvardsson, B., additional, Jönsson, H., additional, Pickering, J. C., additional, Ryde, N., additional, Bayo Arán, A., additional, Bensby, T., additional, Casey, A. R., additional, Feltzing, S., additional, Jofré, P., additional, Korn, A. J., additional, Pancino, E., additional, Damiani, F., additional, Lanzafame, A., additional, Lardo, C., additional, Monaco, L., additional, Morbidelli, L., additional, Smiljanic, R., additional, Worley, C., additional, Zaggia, S., additional, Randich, S., additional, and Gilmore, G. F., additional
Published: 2021
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42. The Gaia-ESO Survey: Calibrating the lithium–age relation with open clusters and associations

Author: Gutiérrez Albarrán, M. L., primary, Montes, D., additional, Gómez Garrido, M., additional, Tabernero, H. M., additional, González Hernández, J. I., additional, Marfil, E., additional, Frasca, A., additional, Lanzafame, A. C., additional, Klutsch, A., additional, Franciosini, E., additional, Randich, S., additional, Smiljanic, R., additional, Korn, A. J., additional, Gilmore, G., additional, Alfaro, E. J., additional, Baratella, M., additional, Bayo, A., additional, Bensby, T., additional, Bonito, R., additional, Carraro, G., additional, Delgado Mena, E., additional, Feltzing, S., additional, Gonneau, A., additional, Heiter, U., additional, Hourihane, A., additional, Jiménez Esteban, F., additional, Jofre, P., additional, Masseron, T., additional, Monaco, L., additional, Morbidelli, L., additional, Prisinzano, L., additional, Roccatagliata, V., additional, Sousa, S., additional, Van der Swaelmen, M., additional, Worley, C. C., additional, and Zaggia, S., additional
Published: 2020
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43. The Gaia-ESO Survey: Spectroscopic-asteroseismic analysis of K2 stars in Gaia-ESO

Author: Worley, C. C., primary, Jofré, P., additional, Rendle, B., additional, Miglio, A., additional, Magrini, L., additional, Feuillet, D., additional, Gavel, A., additional, Smiljanic, R., additional, Lind, K., additional, Korn, A., additional, Gilmore, G., additional, Randich, S., additional, Hourihane, A., additional, Gonneau, A., additional, Francois, P., additional, Lewis, J., additional, Sacco, G., additional, Bragaglia, A., additional, Heiter, U., additional, Feltzing, S., additional, Bensby, T., additional, Irwin, M., additional, Gonzalez Solares, E., additional, Murphy, D., additional, Bayo, A., additional, Sbordone, L., additional, Zwitter, T., additional, Lanzafame, A. C., additional, Walton, N., additional, Zaggia, S., additional, Alfaro, E. J., additional, Morbidelli, L., additional, Sousa, S., additional, Monaco, L., additional, Carraro, G., additional, and Lardo, C., additional
Published: 2020
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44. The Gaia-ESO Survey: Galactic evolution of lithium at high metallicity

Author: Randich, S., primary, Pasquini, L., additional, Franciosini, E., additional, Magrini, L., additional, Jackson, R. J., additional, Jeffries, R. D., additional, d’Orazi, V., additional, Romano, D., additional, Sanna, N., additional, Tautvaišienė, G., additional, Tsantaki, M., additional, Wright, N. J., additional, Gilmore, G., additional, Bensby, T., additional, Bragaglia, A., additional, Pancino, E., additional, Smiljanic, R., additional, Bayo, A., additional, Carraro, G., additional, Gonneau, A., additional, Hourihane, A., additional, Morbidelli, L., additional, and Worley, C. C., additional
Published: 2020
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45. The Gaia-ESO Survey: an extremely Li-rich giant in globular cluster NGC 1261

Author: Sanna, N., primary, Franciosini, E., additional, Pancino, E., additional, Mucciarelli, A., additional, Tsantaki, M., additional, Charbonnel, C., additional, Smiljanic, R., additional, Fu, X., additional, Bragaglia, A., additional, Lagarde, N., additional, Tautvaišiene, G., additional, Magrini, L., additional, Randich, S., additional, Bensby, T., additional, Korn, A. J., additional, Bayo, A., additional, Bergemann, M., additional, Carraro, G., additional, and Morbidelli, L., additional
Published: 2020
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46. The Gaia-ESO survey: the non-universality of the age–chemical-clocks–metallicity relations in the Galactic disc

Author: Casali, G., primary, Spina, L., additional, Magrini, L., additional, Karakas, A. I., additional, Kobayashi, C., additional, Casey, A. R., additional, Feltzing, S., additional, Van der Swaelmen, M., additional, Tsantaki, M., additional, Jofré, P., additional, Bragaglia, A., additional, Feuillet, D., additional, Bensby, T., additional, Biazzo, K., additional, Gonneau, A., additional, Tautvaišienė, G., additional, Baratella, M., additional, Roccatagliata, V., additional, Pancino, E., additional, Sousa, S., additional, Adibekyan, V., additional, Martell, S., additional, Bayo, A., additional, Jackson, R. J., additional, Jeffries, R. D., additional, Gilmore, G., additional, Randich, S., additional, Alfaro, E., additional, Koposov, S. E., additional, Korn, A. J., additional, Recio-Blanco, A., additional, Smiljanic, R., additional, Franciosini, E., additional, Hourihane, A., additional, Monaco, L., additional, Morbidelli, L., additional, Sacco, G., additional, Worley, C., additional, and Zaggia, S., additional
Published: 2020
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47. The Gaia-ESO Survey: a new approach to chemically characterising young open clusters

Author: Baratella, M., primary, D’Orazi, V., additional, Carraro, G., additional, Desidera, S., additional, Randich, S., additional, Magrini, L., additional, Adibekyan, V., additional, Smiljanic, R., additional, Spina, L., additional, Tsantaki, M., additional, Tautvaišienė, G., additional, Sousa, S. G., additional, Jofré, P., additional, Jiménez-Esteban, F. M., additional, Delgado-Mena, E., additional, Martell, S., additional, Van der Swaelmen, M., additional, Roccatagliata, V., additional, Gilmore, G., additional, Alfaro, E. J., additional, Bayo, A., additional, Bensby, T., additional, Bragaglia, A., additional, Franciosini, E., additional, Gonneau, A., additional, Heiter, U., additional, Hourihane, A., additional, Jeffries, R. D., additional, Koposov, S. E., additional, Morbidelli, L., additional, Prisinzano, L., additional, Sacco, G., additional, Sbordone, L., additional, Worley, C., additional, Zaggia, S., additional, and Lewis, J., additional
Published: 2020
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48. Lithium in red giant stars: Constraining non-standard mixing with large surveys in the Gaia era

Author: Charbonnel, C., primary, Lagarde, N., additional, Jasniewicz, G., additional, North, P. L., additional, Shetrone, M., additional, Krugler Hollek, J., additional, Smith, V. V., additional, Smiljanic, R., additional, Palacios, A., additional, and Ottoni, G., additional
Published: 2020
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49. The gaia -ESO survey: calibration strategy

Author: Pancino, E., Lardo, C., Altavilla, G., Marinoni, S., Ragaini, S., Cocozza, G., Bellazzini, M., Sabbi, E., Zoccali, M., Donati, P., Heiter, U., Koposov, S. E., Blomme, R., Morel, T., Símon-Díaz, S., Lobel, A., Soubiran, C., Montalban, J., Valentini, M., Casey, A. R., Blanco-Cuaresma, S., Jofré, P., Worley, C. C., Magrini, L., Hourihane, A., François, P., Feltzing, S., Gilmore, G., Randich, S., Asplund, M., Bonifacio, P., Drew, J. E., Jeffries, R. D., Micela, G., Vallenari, A., Alfaro, E. J., Allende Prieto, C., Babusiaux, C., Bensby, T., angela Bragaglia, Flaccomio, E., Hambly, N., Korn, A. J., Lanzafame, A. C., Smiljanic, R., Eck, S., Walton, N. A., Bayo, A., Carraro, G., Costado, M. T., Damiani, F., Edvardsson, B., Franciosini, E., Frasca, A., Lewis, J., Monaco, L., Morbidelli, L., Prisinzano, L., Sacco, G. G., Sbordone, L., Sousa, S. G., Zaggia, S., Koch, A., Ministero dell'Istruzione, dell'Università e della Ricerca, Knut and Alice Wallenberg Foundation, European Research Council, Swedish National Space Board, Belgian Science Policy Office, National Science Centre (Poland), European Science Foundation, Ministerio de Economía y Competitividad (España), Pancino E., Lardo C., Altavilla G., Marinoni S., Ragaini S., Cocozza G., Bellazzini M., Sabbi E., Zoccali M., Donati P., Heiter U., Koposov S.E., Blomme R., Morel T., Simon-Diaz S., Lobel A., Soubiran C., Montalban J., Valentini M., Casey A.R., Blanco-Cuaresma S., Jofre P., Worley C.C., Magrini L., Hourihane A., Francois P., Feltzing S., Gilmore G., Randich S., Asplund M., Bonifacio P., Drew J.E., Jeffries R.D., Micela G., Vallenari A., Alfaro E.J., Allende Prieto C., Babusiaux C., Bensby T., Bragaglia A., Flaccomio E., Hambly N., Korn A.J., Lanzafame A.C., Smiljanic R., Van Eck S., Walton N.A., Bayo A., Carraro G., Costado M.T., Damiani F., Edvardsson B., Franciosini E., Frasca A., Lewis J., Monaco L., Morbidelli L., Prisinzano L., Sacco G.G., Sbordone L., Sousa S.G., Zaggia S., Koch A., Institut national de recherche et de sécurité (Vandoeuvre lès Nancy) (INRS ( Vandoeuvre lès Nancy)), Royal Observatory of Belgium [Brussels] (ROB), Science et Ingénierie des Matériaux et Procédés (SIMaP ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), M2A 2017, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Leibniz-Institut für Astrophysik Potsdam (AIP), Focas Research Institute, Dublin Institute of Technology, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), School of Physics, Astronomy and Mathematics [Hatfield], University of Hertfordshire [Hatfield] (UH), INAF - Osservatorio Astronomico di Palermo (OAPa), Istituto Nazionale di Astrofisica (INAF), Economía Política y Hacienda Pública, Estadística Económica y Empresarial y Política Económica, Universidad de Castilla-La Mancha (UCLM), Department of Astronomy and Space Physics [Uppsala], Uppsala University, INAF - Osservatorio Astrofisico di Catania (OACT), Institut d'Astronomie et d'Astrophysique, Université libre de Bruxelles (ULB), University of Turin, Department of Physiology and Pharmacology, Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome]-Réseau International des Instituts Pasteur (RIIP)-Institut Pasteur, Fondation Cenci Bolognetti - Istituto Pasteur Italia, Fondazione Cenci Bolognetti, Réseau International des Instituts Pasteur (RIIP), Pôle Gérontologie, and Centre Hospitalier Universitaire de Nice (CHU Nice)
Subjects: Stars: abundance, Milky Way, FOS: Physical sciences, Techniques: spectroscopic, Astrophysics, Parameter space, Surveys, 01 natural sciences, Spectral line, surveys, 0103 physical sciences, Calibration, Emission spectrum, Survey, 010303 astronomy & astrophysics, Galaxy: general, Solar and Stellar Astrophysics (astro-ph.SR), QC, general [Galaxy], QB, Physics, [PHYS]Physics [physics], Observational error, 010308 nuclear & particles physics, Techniques: radial velocitie, Stars: abundances, Astronomy and Astrophysics, Ranging, radial velocities [techniques], [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Astrophysics of Galaxies, abundances [stars], Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Techniques: radial velocities, stars: abundances, techniques: spectroscopic, techniques: radial velocities, spectroscopic [techniques], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: The Gaia-ESO survey (GES) is now in its fifth and last year of observations and has produced tens of thousands of high-quality spectra of stars in all Milky Way components. This paper presents the strategy behind the selection of astrophysical calibration targets, ensuring that all GES results on radial velocities, atmospheric parameters, and chemical abundance ratios will be both internally consistent and easily comparable with other literature results, especially from other large spectroscopic surveys and from Gaia. The calibration of GES is particularly delicate because of (i) the large space of parameters covered by its targets, ranging from dwarfs to giants, from O to M stars; these targets have a large wide of metallicities and also include fast rotators, emission line objects, and stars affected by veiling; (ii) the variety of observing setups, with different wavelength ranges and resolution; and (iii) the choice of analyzing the data with many different state-of-the-art methods, each stronger in a different region of the parameter space, which ensures a better understanding of systematic uncertainties. An overview of the GES calibration and homogenization strategy is also given, along with some examples of the usage and results of calibrators in GES iDR4, which is the fourth internal GES data release and will form the basis of the next GES public data release. The agreement between GES iDR4 recommended values and reference values for the calibrating objects are very satisfactory. The average offsets and spreads are generally compatible with the GES measurement errors, which in iDR4 data already meet the requirements set by the main GES scientific goals.© ESO, 2017., This work was partly supported by the European Union FP7 program through ERC grant number 320360 and by the Leverhulme Trust through grant RPG-2012-541. We acknowledge the support from INAF and Ministero dell'Istruzione, dell'Universita e della Ricerca (MIUR) in the form of the grant >Premiale VLT 2012>. The results presented here benefit from discussions held during the Gaia-ESO workshops and conferences supported by the ESF (European Science Foundation) through the GREAT Research Network Programme. S.F. and T.B. acknowledge the support from the New Milky Way project funded by a grant from the Knut and Alice Wallenberg foundation. C.L. gratefully acknowledges financial support from the European Research Council (ERC-CoG-646928, Multi-Pop, PI: N. Bastian). U.H. and A.J.K acknowledge support from the Swedish National Space Board (Rymdstyrelsen). The research of A.L. has been subsidized by the Belgian Federal Science Policy Office under contract No. BR/143/A2/BRASS. R.S. acknowledges support by the National Science Center of Poland through grant 2014/15/B/ST9/03981. C.A.P. is thankful for support from the Spanish Ministry of Economy and Competitiveness (MINECO) through grant AYA2014-56359-P.J.M. acknowledges support from the ERC Consolidator Grant funding scheme (project STARKEY, G.A. No. 615604). T.M. acknowledges financial support from Belspo for contract PRODEX Gaia-DPAC. S.G.S acknowledges the support by Fundacao para a Ciencia e Tecnologia (FCT) through national funds and a research grant (project ref. UID/FIS/04434/2013, and PTDC/FIS-AST/7073/2014). S.G.S. also acknowledge the support from FCT through Investigador FCT contract of reference IF/00028/2014 and POPH/FSE (EC) by FEDER funding through the program >Programa Operacional de Factores de Competitividade - COMPETE>. L.S. acknowledges support by the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics (MAS). M.Z. acknowledges support by the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics (MAS), by Fondecyt Regular 1150345 and by the BASAL CATA PFB-06. E.J.A. and M.T.C acknowledge the financial support from the Spanish Ministerio de Economia y Competitividad, through grant AYA2013-40611-P.S.Z. acknowledge the support from the INAF grant >PRIN INAF 2014>, >Star won't tell their ages to Gaia, Galactic Archaelogy with wide-area asterosismic>.
Published: 2017

50. The Gaia -ESO Survey: open clusters in Gaia -DR1

Author: Randich, S., Tognelli, E., Jackson, R., Jeffries, R., Degl’Innocenti, S., Pancino, E., Fiorentin, P. Re, Spagna, A., Sacco, G., Bragaglia, A., Magrini, L., Moroni, G., Alfaro, E., Franciosini, E., Morbidelli, L., Roccatagliata, V., Bouy, H., Bravi, L., Jiménez-Esteban, F., Jordi, C., Zari, E., Tautvaišiene, G., Drazdauskas, A., Mikolaitis, S., Gilmore, G., Feltzing, S., Vallenari, A., Bensby, T., Koposov, S., Korn, A., Lanzafame, A., Smiljanic, R., Bayo, A., Carraro, G., Costado, T., Heiter, U., Hourihane, A., Jofre, P., Lewis, J., Monaco, L., Prisinzano, L., Sbordone, L., Sousa, S., Worley, C., Zaggia, S., INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), M2A 2018, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Ciencies del Cosmos (ICCUB), Universitat de Barcelona (UB), Lund Observatory, Lund University [Lund], INAF - Osservatorio Astrofisico di Catania (OACT), Uppsala University, Istituto Nazionale di Fisica Nucleare, Sezione di Milano (INFN), Istituto Nazionale di Fisica Nucleare (INFN), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: parallaxes - surveys - stars: evolution - open clusters and associations: general, ComputingMilieux_MISCELLANEOUS, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract: International audience
Published: 2018

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